From 12cd58b78eed1b75bfbb255c3d7ad8330876ee04 Mon Sep 17 00:00:00 2001 From: czsky Date: Sun, 1 Oct 2023 16:46:32 +0000 Subject: [PATCH] Updates --- cs/constellation/cancer.md | 8 ++++---- cs/constellation/indus.md | 8 ++++---- cs/constellation/mensa.md | 8 ++++---- cs/constellation/pictor.md | 8 ++++---- cs/constellation/pyxis.md | 8 ++++---- cs/constellation/telescopium.md | 8 ++++---- cs/dso/Abell/Abell10.md | 2 +- cs/dso/Abell/Abell10_100u150.md | 4 ++-- cs/dso/Abell/Abell10_200u250.md | 4 ++-- cs/dso/Abell/Abell10_300u350.md | 4 ++-- cs/dso/Abell/Abell10_400u500.md | 4 ++-- cs/dso/Abell/Abell12.md | 2 +- cs/dso/Abell/Abell12_100u150.md | 4 ++-- cs/dso/Abell/Abell12_200u250.md | 4 ++-- cs/dso/Abell/Abell12_400u500.md | 4 ++-- cs/dso/Abell/Abell12_600u800.md | 4 ++-- cs/dso/Abell/Abell13.md | 2 +- cs/dso/Abell/Abell13_400u500.md | 10 +++++----- cs/dso/Abell/Abell13_600u800.md | 4 ++-- cs/dso/Abell/Abell20_200u250.md | 6 +++--- cs/dso/Abell/Abell20_400u500.md | 6 +++--- cs/dso/Abell/Abell20_600u800.md | 4 ++-- cs/dso/Cr/Cr132.md | 12 ++++++------ cs/dso/Jonckheere/Jonckheere320.md | 6 +++--- cs/dso/Jonckheere/Jonckheere320_400u500.md | 4 ++-- cs/dso/M/M1.md | 20 ++++++++++---------- cs/dso/M/M1_200u250.md | 4 ++-- cs/dso/M/M1_300u350.md | 2 +- cs/dso/M/M1_400u500.md | 2 +- cs/dso/M/M1_600u800.md | 4 ++-- cs/dso/M/M45.md | 16 ++++++++-------- cs/dso/NGC/1400-1500/NGC1409.md | 9 +++++++++ cs/dso/NGC/1400-1500/NGC1409_400u500.md | 9 +++++++++ cs/dso/NGC/1500-1600/NGC1555.md | 9 +++++++++ cs/dso/NGC/1500-1600/NGC1555_400u500.md | 9 +++++++++ cs/dso/NGC/1500-1600/NGC1555_600u800.md | 9 +++++++++ cs/dso/NGC/1500-1600/NGC1555_900u1200.md | 9 +++++++++ cs/dso/NGC/1500-1600/NGC1587.md | 9 +++++++++ cs/dso/NGC/1500-1600/NGC1587_300u350.md | 9 +++++++++ cs/dso/NGC/1500-1600/NGC1587_400u500.md | 9 +++++++++ cs/dso/NGC/1700-1800/NGC1750.md | 9 +++++++++ cs/dso/NGC/1700-1800/NGC1750_400u500.md | 9 +++++++++ cs/dso/NGC/1800-1900/NGC1819.md | 9 +++++++++ cs/dso/NGC/1800-1900/NGC1819_300u350.md | 9 +++++++++ cs/dso/NGC/1900-2000/NGC1973.md | 6 +++--- cs/dso/NGC/1900-2000/NGC1973_300u350.md | 4 ++-- cs/dso/NGC/2000-2100/NGC2071.md | 2 +- cs/dso/NGC/2000-2100/NGC2071_200u250.md | 4 ++-- cs/dso/NGC/2000-2100/NGC2071_400u500.md | 6 +++--- cs/dso/NGC/2100-2200/IC2162.md | 2 +- cs/dso/NGC/2100-2200/IC2162_400u500.md | 4 ++-- cs/dso/NGC/2100-2200/IC2162_600u800.md | 2 +- cs/dso/NGC/2100-2200/IC2177.md | 4 ++-- cs/dso/NGC/2100-2200/IC2177_300u350.md | 2 +- cs/dso/NGC/2100-2200/NGC2175.md | 2 +- cs/dso/NGC/2100-2200/NGC2175_300u350.md | 2 +- cs/dso/NGC/2100-2200/NGC2175_400u500.md | 2 +- cs/dso/NGC/2300-2400/IC2375.md | 9 +++++++++ cs/dso/NGC/2300-2400/IC2375_400u500.md | 9 +++++++++ cs/dso/NGC/2300-2400/IC2375_600u800.md | 11 +++++++++++ cs/dso/NGC/2300-2400/NGC2345.md | 4 ++-- cs/dso/NGC/2300-2400/NGC2345_200u250.md | 2 +- cs/dso/NGC/2300-2400/NGC2345_300u350.md | 4 ++-- cs/dso/NGC/2300-2400/NGC2392.md | 6 +++--- cs/dso/NGC/2300-2400/NGC2392_200u250.md | 6 +++--- cs/dso/NGC/2300-2400/NGC2392_400u500.md | 4 ++-- cs/dso/NGC/2400-2500/NGC2479.md | 9 +++++++++ cs/dso/NGC/2400-2500/NGC2479_300u350.md | 9 +++++++++ cs/dso/NGC/2400-2500/NGC2479_400u500.md | 9 +++++++++ cs/dso/NGC/2400-2500/NGC2489.md | 9 +++++++++ cs/dso/NGC/2400-2500/NGC2489_300u350.md | 9 +++++++++ cs/dso/NGC/2500-2600/NGC2525.md | 9 +++++++++ cs/dso/NGC/2500-2600/NGC2525_300u350.md | 9 +++++++++ cs/dso/NGC/2500-2600/NGC2525_600u800.md | 9 +++++++++ cs/dso/NGC/2500-2600/NGC2568.md | 9 +++++++++ cs/dso/NGC/2500-2600/NGC2568_300u350.md | 9 +++++++++ cs/dso/NGC/2500-2600/NGC2571.md | 9 +++++++++ cs/dso/NGC/2500-2600/NGC2571_300u350.md | 9 +++++++++ cs/dso/NGC/2500-2600/NGC2571_400u500.md | 9 +++++++++ cs/dso/NGC/300-400/IC349.md | 9 +++++++++ cs/dso/NGC/300-400/IC349_900u1200.md | 9 +++++++++ cs/dso/NGC/3000-3100/NGC3047.md | 9 +++++++++ cs/dso/NGC/3000-3100/NGC3047_400u500.md | 9 +++++++++ cs/dso/NGC/3100-3200/NGC3156.md | 9 +++++++++ cs/dso/NGC/3100-3200/NGC3156_300u350.md | 9 +++++++++ cs/dso/NGC/3100-3200/NGC3156_400u500.md | 9 +++++++++ cs/dso/NGC/3100-3200/NGC3166_400u500.md | 4 ++-- cs/dso/NGC/3200-3300/NGC3247.md | 9 +++++++++ cs/dso/NGC/3200-3300/NGC3247_300u350.md | 9 +++++++++ cs/dso/NGC/3300-3400/NGC3372.md | 16 ++++++++-------- cs/dso/NGC/3300-3400/NGC3372_300u350.md | 2 +- cs/dso/NGC/400-500/IC412.md | 9 +++++++++ cs/dso/NGC/400-500/IC412_400u500.md | 9 +++++++++ cs/dso/NGC/400-500/IC412_600u800.md | 11 +++++++++++ cs/dso/NGC/400-500/IC447.md | 9 +++++++++ cs/dso/NGC/400-500/IC447_400u500.md | 9 +++++++++ cs/dso/NGC/4300-4400/NGC4314_400u500.md | 4 ++-- cs/dso/NGC/500-600/IC575.md | 9 +++++++++ cs/dso/NGC/500-600/IC575_400u500.md | 9 +++++++++ cs/dso/NGC/500-600/IC575_900u1200.md | 11 +++++++++++ cs/dso/Sh2/Sh2-276.md | 22 +++++++++++----------- cs/dso/UGC/UGC3573_600u800.md | 6 +++--- cs/star/Dunlop_236.md | 6 +++--- cs/star/hr1175.md | 6 +++--- cs/star/hr1336.md | 4 ++-- cs/star/hr1355.md | 6 +++--- cs/star/hr1605.md | 4 ++-- cs/star/hr183.md | 6 +++--- cs/star/hr191.md | 6 +++--- cs/star/hr2020.md | 6 +++--- cs/star/hr3433.md | 6 +++--- cs/star/hr3438.md | 6 +++--- cs/star/hr3541.md | 4 ++-- cs/star/hr3628.md | 6 +++--- cs/star/hr3644.md | 6 +++--- cs/star/hr6072.md | 6 +++--- cs/star/hr6115.md | 6 +++--- en/constellation/antlia.md | 8 ++++---- en/constellation/apus.md | 6 +++--- en/constellation/ara.md | 6 +++--- en/constellation/auriga.md | 6 +++--- en/constellation/cancer.md | 6 +++--- en/constellation/canis major.md | 6 +++--- en/constellation/canis minor.md | 6 +++--- en/constellation/carina.md | 10 +++++----- en/constellation/centaurus.md | 10 +++++----- en/constellation/chamaeleon.md | 6 +++--- en/constellation/circinus.md | 10 +++++----- en/constellation/columba.md | 6 +++--- en/constellation/dorado.md | 6 +++--- en/constellation/grus.md | 6 +++--- en/constellation/hydrus.md | 6 +++--- en/constellation/indus.md | 6 +++--- en/constellation/mensa.md | 6 +++--- en/constellation/microscopium.md | 6 +++--- en/constellation/musca.md | 6 +++--- en/constellation/norma.md | 6 +++--- en/constellation/octans.md | 6 +++--- en/constellation/pavo.md | 6 +++--- en/constellation/phoenix.md | 8 ++++---- en/constellation/pictor.md | 8 ++++---- en/constellation/pyxis.md | 6 +++--- en/constellation/reticulum.md | 8 ++++---- en/constellation/telescopium.md | 6 +++--- en/constellation/tucana.md | 8 ++++---- en/star/38_Psc.md | 8 -------- en/star/Barnard's_Star.md | 9 --------- en/star/Brisbane_14.md | 9 --------- en/star/Burnham_441.md | 9 --------- en/star/Burnham_800.md | 9 --------- en/star/CAS_A.md | 9 --------- en/star/Cygnus_X-1.md | 9 --------- en/star/Dunlop_236.md | 8 -------- en/star/False_Cross.md | 9 --------- en/star/Groombridge_1830.md | 9 --------- en/star/Groombridge_34_(Grb_34).md | 9 --------- en/star/Herschel_3750.md | 9 --------- en/star/Herschel_3780.md | 9 --------- en/star/Herschel_3857.md | 9 --------- en/star/Herschel_4423.md | 9 --------- en/star/Herschel_4788.md | 9 --------- en/star/Herschel_5003.md | 9 --------- en/star/Herschel_84.md | 9 --------- en/star/Hind's_Crimson_Star_(R_Lep).md | 9 --------- en/star/Kapteynova_hviezda.md | 8 -------- en/star/Keplerova_supernova.md | 9 --------- en/star/Kruger_60.md | 9 --------- en/star/Lacaille_9352.md | 9 --------- en/star/Lalande_21185.md | 9 --------- en/star/Musca_Borealis.md | 9 --------- en/star/N_1918_Aql.md | 9 --------- en/star/N_1991.md | 8 -------- en/star/N_Hya.md | 9 --------- en/star/Nova_Delphini_1967.md | 9 --------- en/star/P_Hya.md | 9 --------- en/star/Plaskett_star.md | 9 --------- en/star/Proxima_Centauri.md | 11 ----------- en/star/RR_Lyrae.md | 9 --------- en/star/RR_Tel.md | 9 --------- en/star/RS_Oph.md | 9 --------- en/star/RW_Tauri.md | 9 --------- en/star/RX_J185635-3754.md | 9 --------- en/star/R_Ara.md | 9 --------- en/star/R_Cae.md | 9 --------- en/star/R_Casiopeiae.md | 9 --------- en/star/R_Com.md | 9 --------- en/star/R_Corvi.md | 9 --------- en/star/R_Hydrae.md | 9 --------- en/star/R_LMi.md | 9 --------- en/star/R_Oct.md | 8 -------- en/star/R_Ret.md | 9 --------- en/star/R_TrA.md | 9 --------- en/star/R_a_S_Gru.md | 8 -------- en/star/R_a_TW_Hor.md | 8 -------- en/star/SN1987A.md | 9 --------- en/star/SN_1006.md | 9 --------- en/star/SS_Cygni.md | 9 --------- en/star/SX_Phe.md | 8 -------- en/star/S_Aps.md | 9 --------- en/star/S_Doradus.md | 9 --------- en/star/S_Vol.md | 9 --------- en/star/S_a_U_Oct.md | 8 -------- en/star/Struve_1095.md | 9 --------- en/star/Struve_1104.md | 9 --------- en/star/Struve_1149.md | 9 --------- en/star/Struve_1441.md | 9 --------- en/star/Struve_1788.md | 9 --------- en/star/Struve_2303.md | 9 --------- en/star/Struve_2306.md | 9 --------- en/star/Struve_2373.md | 9 --------- en/star/Struve_2455.md | 9 --------- en/star/Struve_2470-slash-2474.md | 9 --------- en/star/Struve_2540.md | 9 --------- en/star/Struve_2653.md | 9 --------- en/star/Struve_2793.md | 9 --------- en/star/Struve_2902.md | 9 --------- en/star/Struve_475.md | 9 --------- en/star/Sualocin_a_Rotanev.md | 9 --------- en/star/Sírius_B.md | 9 --------- en/star/T_Borealis.md | 8 -------- en/star/T_Col.md | 9 --------- en/star/T_Pyxidis.md | 8 -------- en/star/T_Tauri.md | 9 --------- en/star/Trapezium.md | 9 --------- en/star/Tycho's_Supernova.md | 9 --------- en/star/UV_Aur.md | 9 --------- en/star/U_Ara.md | 9 --------- en/star/U_Cep.md | 9 --------- en/star/VW_Hyi.md | 8 -------- en/star/V_Hya.md | 9 --------- en/star/V_Sge.md | 9 --------- en/star/Van_Maanenova_hviezda.md | 8 -------- en/star/W_a_X_Sgr.md | 9 --------- en/star/Wolf_359.md | 9 --------- en/star/Wolf_457.md | 8 -------- en/star/Z_Cam.md | 9 --------- en/star/Z_Cha.md | 9 --------- en/star/h3945.md | 9 --------- en/star/hr1010.md | 9 --------- en/star/hr1017.md | 8 -------- en/star/hr1084.md | 8 -------- en/star/hr1175.md | 9 --------- en/star/hr1203.md | 8 -------- en/star/hr1208.md | 8 -------- en/star/hr1212.md | 8 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| 9 --------- en/star/hr2588.md | 9 --------- en/star/hr2593.md | 9 --------- en/star/hr2618.md | 9 --------- en/star/hr264.md | 9 --------- en/star/hr2650.md | 9 --------- en/star/hr2671.md | 9 --------- en/star/hr2736.md | 9 --------- en/star/hr2742.md | 9 --------- en/star/hr2748.md | 9 --------- en/star/hr2777.md | 9 --------- en/star/hr2782.md | 9 --------- en/star/hr2784.md | 9 --------- en/star/hr280.md | 9 --------- en/star/hr2878.md | 9 --------- en/star/hr2891.md | 9 --------- en/star/hr2943.md | 9 --------- en/star/hr2990.md | 9 --------- en/star/hr310.md | 8 -------- en/star/hr3110.md | 9 --------- en/star/hr3165.md | 9 --------- en/star/hr3188.md | 9 --------- en/star/hr3207.md | 9 --------- en/star/hr3208.md | 9 --------- en/star/hr322.md | 8 -------- en/star/hr3223.md | 9 --------- en/star/hr3248.md | 9 --------- en/star/hr3301.md | 9 --------- en/star/hr3318.md | 9 --------- en/star/hr3340.md | 9 --------- en/star/hr3347.md | 9 --------- en/star/hr338.md | 8 -------- 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Obrácené "Y" leží ve středu rovnostranného trojúhelníku, který utvářejí hvězdy Pollux, Regulus a Prokyon. Tvoří ho hvězdy Altarf, Acubens, Asellus Australus, ι a χ Cancri. Před 2000 lety Slunce procházelo Rakem v době letního slunovratu, bylo tedy nejsevernějším souhvězdím zvířetníku. V současnosti jím prochází od 20. července do 9. srpna. Znakem Raka se ale stále označuje letní slunovrat a obratník severní polokoule se nazývá obratníkem Raka. V současnosti vystupuje Slunce nejvýše na severní polokouli na rozhraní souhvězdí Blíženců a Býka. Rak je nejméně výrazným souhvězdím zvířetníku, jen jedna jeho hvězda přesahuje 4. magnitudu. Bezměsíčná noc je proto podmínkou, abychom souhvězdí na obloze co nejlépe viděli. Rak se pyšní dvěmi otevřenými hvězdokupami, jedněmi z nejkrásnějších na celé obloze. Tou jasnější je M44, ležící téměř ve středu souhvězdí. V dávných dobách, v roce 270 před n. l. ji nazval "Praesepe" (Jesličky) řecký básník Aratus. Od té doby uplynulo již několik století, kdy je v roce 1610 poprvé dalekohledem rozlišil na jednotlivé hvězdy Galileo Galilei. V současnosti nám na tom bude stačit i obyčejný triedr. V souhvězdí je také několik dvojhvězd a protože se nachází dále od Mléčné dráhy, najdeme v něm i větší počet slabších galaxií. - -![<]($IMG_DIR/cons/Cnc.png) +Nevýrazné souhvězdí severní oblohy mezi Blíženci a Lvem. Obrácené "Y" leží ve středu rovnostranného trojúhelníku, který utvářejí hvězdy Pollux, Regulus a Prokyon. Tvoří ho hvězdy Altarf, Acubens, Asellus Australus, ι a χ Cancri. Před 2000 lety Slunce procházelo Rakem v době letního slunovratu, bylo tedy nejsevernějším souhvězdím zvířetníku. V současnosti jím prochází od 20. července do 9. srpna. Znakem Raka se ale stále označuje letní slunovrat a obratník severní polokoule se nazývá obratníkem Raka. V současnosti vystupuje Slunce nejvýše na severní polokouli na rozhraní souhvězdí Blíženců a Býka. Rak je nejméně výrazným souhvězdím zvířetníku, jen jedna jeho hvězda přesahuje 4. magnitudu. Bezměsíčná noc je proto podmínkou, abychom souhvězdí na obloze viděli co nejlépe. Rak se pyšní dvěmi otevřenými hvězdokupami, jedněmi z nejkrásnějších na celé obloze. Tou jasnější je M44, ležící téměř ve středu souhvězdí. V dávných dobách, v roce 270 před n. l. ji nazval "Praesepe" (Jesličky) řecký básník Aratus. Od té doby uplynulo již několik století, kdy je v roce 1610 poprvé dalekohledem rozlišil na jednotlivé hvězdy Galileo Galilei. V současnosti nám na tom bude stačit i obyčejný triedr. V souhvězdí je také několik dvojhvězd a protože se nachází dále od Mléčné dráhy, najdeme v něm i větší počet slabších galaxií. + +![<]($IMG_DIR/cons/Cnc.png) diff --git a/cs/constellation/indus.md b/cs/constellation/indus.md index 8c66c5da8..b9367ac6a 100644 --- a/cs/constellation/indus.md +++ b/cs/constellation/indus.md @@ -3,8 +3,8 @@ name: Indián created_by: editor.cs created_date: 2020-09-23 20:52:20.271846 updated_by: skybber -updated_date: 2020-09-23 20:52:20.271862 +updated_date: 2022-12-29 10:40:57.629331 --- -![<]($IMG_DIR/cons/Ind.png) -Malé a nevýrazné souhvězdí jižní oblohy obklopené trojicí opeřenců: Jeřábem, tukan, Pavem a zabíhající až do blízkosti jižního pólu oblohy. Asi těžko se dá v několika nejasných hvězdách tohoto souhvězdí představit severoamerický indián. Jako orientační pomůcka k vyhledání souhvězdí může posloužit o něco nápadnější Páv, jehož nejjasnější hvězda Peacock leží v těsném sousedství Indiána. U nás toto souhvězdí není viditelné. - +![<]($IMG_DIR/cons/Ind.png) +Malé a nevýrazné souhvězdí jižní oblohy obklopené trojicí opeřenců: Jeřábem, Tukanem, Pavem a zabíhající až do blízkosti jižního pólu oblohy. Asi těžko se dá v několika nejasných hvězdách tohoto souhvězdí představit severoamerický indián. Jako orientační pomůcka k vyhledání souhvězdí může posloužit o něco nápadnější Páv, jehož nejjasnější hvězda Peacock leží v těsném sousedství Indiána. U nás toto souhvězdí není viditelné. + diff --git a/cs/constellation/mensa.md b/cs/constellation/mensa.md index 4fa43c9e5..bb23e6f94 100644 --- a/cs/constellation/mensa.md +++ b/cs/constellation/mensa.md @@ -3,8 +3,8 @@ name: Stolová hora created_by: editor.cs created_date: 2020-09-23 20:52:20.320395 updated_by: skybber -updated_date: 2020-09-23 20:52:20.320410 +updated_date: 2022-12-29 11:28:06.431422 --- -![<]($IMG_DIR/cons/Men.png) -Malé a nevýrazné souhvězdí v těsném sousedství jižního pólu oblohy, v našich zeměpisných šířkách proto není viditelné. Stolní vrch je nejslabším souhvězdím oblohy, jehož nejjasnější hvězdy nepřevyšují pátou magnitudu. Čtyři z nich tvoří hlavní obrazec souhvězdí. Z objektů za zmínku stojí pouze Velký Magellanův mrak, který sem ze severu částečně zasahuje ze sousedního Mečiara. - +![<]($IMG_DIR/cons/Men.png) +Malé a nevýrazné souhvězdí v těsném sousedství jižního pólu oblohy, v našich zeměpisných šířkách proto není viditelné. Stolní vrch je nejslabším souhvězdím oblohy, jehož nejjasnější hvězdy nepřevyšují pátou magnitudu. Čtyři z nich tvoří hlavní obrazec souhvězdí. Z objektů za zmínku stojí pouze Velký Magellanův mrak, který sem ze severu částečně zasahuje ze sousedního Mečouna. + diff --git a/cs/constellation/pictor.md b/cs/constellation/pictor.md index e248b5051..11e99ce37 100644 --- a/cs/constellation/pictor.md +++ b/cs/constellation/pictor.md @@ -3,8 +3,8 @@ name: Malíř created_by: editor.cs created_date: 2020-09-23 20:52:20.057938 updated_by: skybber -updated_date: 2020-09-23 20:52:20.057959 +updated_date: 2023-01-02 17:49:19.032631 --- -Menší a nevýraznejšie souhvězdí jižní oblohy, které u nás není viditelné. Tato jednotvárná skupina hvězd leží pod holubici, hned západně od velmi jasné hvězdy Canopus ze souhvězdí kýlu. Nejznámějším objektem tohoto malého jižního souhvězdí je Kapteynova hvězda, červený podtrpaslík nejbližší k Zemi a kosmu. zdroj záření, který lze pozorovat na frekvenci 18,3 MHz. V roce 1925 se v souhvězdí Malíře objevila neobvyklá nova. V době objevu měla 2. magnitudu, postupně se však zjasnila až na 1mag. Pak postupně slábla, aby se opět po dvou měsících od svého prvního maxima zjasnila. - -![<]($IMG_DIR/cons/Pic.png) +Menší a nevýraznejšie souhvězdí jižní oblohy, které u nás není viditelné. Tato jednotvárná skupina hvězd leží pod Holubicí, hned západně od velmi jasné hvězdy Canopus ze souhvězdí Lodního kýlu. Nejznámějším objektem tohoto malého jižního souhvězdí je Kapteynova hvězda, červený podtrpaslík nejbližší k Zemi a kosmu. zdroj záření, který lze pozorovat na frekvenci 18,3 MHz. V roce 1925 se v souhvězdí Malíře objevila neobvyklá nova. V době objevu měla 2. magnitudu, postupně se však zjasnila až na 1mag. Pak postupně slábla, aby se opět po dvou měsících od svého prvního maxima zjasnila. + +![<]($IMG_DIR/cons/Pic.png) diff --git a/cs/constellation/pyxis.md b/cs/constellation/pyxis.md index 7ef77b944..266778085 100644 --- a/cs/constellation/pyxis.md +++ b/cs/constellation/pyxis.md @@ -3,8 +3,8 @@ name: Kompas created_by: editor.cs created_date: 2020-09-23 20:52:20.170756 updated_by: skybber -updated_date: 2020-09-23 20:52:20.170772 +updated_date: 2023-01-03 17:01:32.035983 --- -Malé a nevýrazné souhvězdí jižní oblohy, které se rozkládá asi 35 stupňů pod hlavou Hydry, mezi vývěva a zádi. Nejjasnější hvězdy souhvězdí Kompas α (3,68mag), β (3,97mag) a γ Pyxidis (4,01mag) leží téměř na přímce. Pro pozorovatele s triedru nebo malým dalekohledem je souhvězdí chudé, nachází se zde však pár slabších otevřených hvězdokup, galaxií a planetárních mlhovin. - -![<]($IMG_DIR/cons/Pyx.png) +Malé a nevýrazné souhvězdí jižní oblohy, které se rozkládá asi 35 stupňů pod hlavou Hydry, mezi Vývěvou a Lodní zádí. Nejjasnější hvězdy souhvězdí Kompas α (3,68mag), β (3,97mag) a γ Pyxidis (4,01mag) leží téměř na přímce. Pro pozorovatele s triedrem nebo malým dalekohledem je souhvězdí chudé, nachází se zde však pár slabších otevřených hvězdokup, galaxií a planetárních mlhovin. + +![<]($IMG_DIR/cons/Pyx.png) diff --git a/cs/constellation/telescopium.md b/cs/constellation/telescopium.md index bc4956165..ff92334b3 100644 --- a/cs/constellation/telescopium.md +++ b/cs/constellation/telescopium.md @@ -3,8 +3,8 @@ name: Dalekohled created_by: editor.cs created_date: 2020-09-23 20:52:20.257100 updated_by: skybber -updated_date: 2020-09-23 20:52:20.257116 +updated_date: 2023-01-03 17:15:56.764343 --- -Nevýrazné a malé souhvězdí jižní oblohy, které se v našich zeměpisných šířkách ukrývá stále pod obzorem. Leží jižně od Štíra, Střelce a Jižní koruny, proto na obloze pochopitelně příliš nevyniká. V souhvězdí najdeme několik slabých galaxií, kulovou hvězdokupu a malou planetární mlhovinu. Kuriozitou je, že dnes v souhvězdí chybí γ Telescopii, ze které se stala G Scorpii v ostnaté Štíra, takže současná verze nebeského dalekohledu je oproti představě N. L. Lacaille podstatně kratší. - -![<]($IMG_DIR/cons/Tel.png) +Nevýrazné a malé souhvězdí jižní oblohy, které se v našich zeměpisných šířkách ukrývá stále pod obzorem. Leží jižně od Štíra, Střelce a Jižní koruny, proto na obloze pochopitelně příliš nevyniká. V souhvězdí najdeme několik slabých galaxií, kulovou hvězdokupu a malou planetární mlhovinu. Kuriozitou je, že dnes v souhvězdí chybí γ Telescopii, ze které se stala G Scorpii v ostnu Štíra, takže současná verze nebeského dalekohledu je oproti představě N. L. Lacaille podstatně kratší. + +![<]($IMG_DIR/cons/Tel.png) diff --git a/cs/dso/Abell/Abell10.md b/cs/dso/Abell/Abell10.md index 38a3f53be..2b4fc8a74 100644 --- a/cs/dso/Abell/Abell10.md +++ b/cs/dso/Abell/Abell10.md @@ -1,6 +1,6 @@ --- name: -rating: 1 +rating: 4 references: created_by: skybber created_date: 2020-09-23 20:52:08.489917 diff --git a/cs/dso/Abell/Abell10_100u150.md b/cs/dso/Abell/Abell10_100u150.md index 3a5808ed6..79732c511 100644 --- a/cs/dso/Abell/Abell10_100u150.md +++ b/cs/dso/Abell/Abell10_100u150.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.657032 updated_by: skybber -updated_date: 2020-09-23 20:52:19.657051 +updated_date: 2022-12-07 18:51:43.257737 --- -63x, [OIII], 6m5+ +63x, [OIII], 6m5+ Bez filtru neviditelná. S [OIII] a 44x malé zjasnění, obtížně nepřímo udržitelné. V 63x jasnější, těsně vedle (2 'JZ) slabá hvězda, kulatá bez struktury, těžká. \ No newline at end of file diff --git a/cs/dso/Abell/Abell10_200u250.md b/cs/dso/Abell/Abell10_200u250.md index 9f9c92989..245eaf8a5 100644 --- a/cs/dso/Abell/Abell10_200u250.md +++ b/cs/dso/Abell/Abell10_200u250.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.991687 updated_by: skybber -updated_date: 2020-09-23 20:52:19.991703 +updated_date: 2022-12-07 18:51:43.257815 --- -47x - 80x, [OIII], 6m5 + +47x - 80x, [OIII], 6m5 + V 47x bez filtru není nic vidět , s [OIII] lze vidět malé, plošné zjasnění. V 80x je ploška viditelná i bez filtru. S filtrem lze vidět jasné, přímo viditelné, kulaté zjasnění, které se nachází přibližně uprostřed mezi dvěma hvězdami 12mag. \ No newline at end of file diff --git a/cs/dso/Abell/Abell10_300u350.md b/cs/dso/Abell/Abell10_300u350.md index 7a0701796..6b1da44f8 100644 --- a/cs/dso/Abell/Abell10_300u350.md +++ b/cs/dso/Abell/Abell10_300u350.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.824396 updated_by: skybber -updated_date: 2020-09-23 20:52:19.824413 +updated_date: 2022-12-07 18:51:43.257855 --- -360x, UHC, 7m2 +360x, UHC, 7m2 Jasná již bez filtru v přehlídkovém zvětšení jako malý kulatý bod. PN nereaguje zvlášť dobře na [OIII], lepší s velkým zvětšením a UHC, kulatý, mírně rozptýlený disk, nějaká struktura v disku, obtížně uchopitelná. \ No newline at end of file diff --git a/cs/dso/Abell/Abell10_400u500.md b/cs/dso/Abell/Abell10_400u500.md index e14a1c9a5..98f501256 100644 --- a/cs/dso/Abell/Abell10_400u500.md +++ b/cs/dso/Abell/Abell10_400u500.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.464604 updated_by: skybber -updated_date: 2020-09-23 20:52:19.464621 +updated_date: 2022-12-07 18:51:43.257891 --- -419x, 7m+ +419x, 7m+ Nápadně jasná a mlhová čočkovitá struktura již v přehlídkovém okuláru. Špatně reaguje na filtry, přesně zaoblená s dobře definovanými vnějšími okraji. Plocha vypadá strukturovaně, přičemž struktura je obtížně uchopitelná. Na hranici vnímání se centrální hvězda, objevuje znovu a znovu a velmi slabě, což je potvrzeno vhodným filtrem. Západní část PN je jasnější. \ No newline at end of file diff --git a/cs/dso/Abell/Abell12.md b/cs/dso/Abell/Abell12.md index 580ad8d63..e0e5bba8c 100644 --- a/cs/dso/Abell/Abell12.md +++ b/cs/dso/Abell/Abell12.md @@ -1,6 +1,6 @@ --- name: -rating: 1 +rating: 5 references: created_by: skybber created_date: 2020-09-23 20:52:08.696757 diff --git a/cs/dso/Abell/Abell12_100u150.md b/cs/dso/Abell/Abell12_100u150.md index 0166172bf..4c3ac1748 100644 --- a/cs/dso/Abell/Abell12_100u150.md +++ b/cs/dso/Abell/Abell12_100u150.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.952095 updated_by: skybber -updated_date: 2020-09-23 20:52:19.952110 +updated_date: 2022-12-07 18:51:09.675246 --- -154x, [OIII], 7m+ +154x, [OIII], 7m+ Při velkém zvětšení a [OIII] může být ploška okamžitě oddělena od jasné mu Ori, vypadá plochá, prstenecová struktura není rozpoznatelná. \ No newline at end of file diff --git a/cs/dso/Abell/Abell12_200u250.md b/cs/dso/Abell/Abell12_200u250.md index 6f3c371b0..d1a263075 100644 --- a/cs/dso/Abell/Abell12_200u250.md +++ b/cs/dso/Abell/Abell12_200u250.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.769205 updated_by: skybber -updated_date: 2020-09-23 20:52:19.769221 +updated_date: 2022-12-07 18:51:09.675332 --- -160x, [OIII], Měsíc (54%) +160x, [OIII], Měsíc (54%) Navzdory Měsíci, okamžitě viditelná jako kulatá oblast přímo obrácená k SZ na Mu Ori, prstencová struktura není rozpoznatelná. \ No newline at end of file diff --git a/cs/dso/Abell/Abell12_400u500.md b/cs/dso/Abell/Abell12_400u500.md index 04cc5329b..ce9f20d09 100644 --- a/cs/dso/Abell/Abell12_400u500.md +++ b/cs/dso/Abell/Abell12_400u500.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.839949 updated_by: skybber -updated_date: 2020-09-23 20:52:19.839965 +updated_date: 2022-12-07 18:51:09.675401 --- -230x, [OIII], 6m6 +230x, [OIII], 6m6 Bez filtru neviditelná, Mu Ori přezařuje PN, okamžitě znatelná s [OIII], tvar prstenu těžký a pouze náznakem, žádná centrální hvězda. \ No newline at end of file diff --git a/cs/dso/Abell/Abell12_600u800.md b/cs/dso/Abell/Abell12_600u800.md index 7049d283b..7887a6906 100644 --- a/cs/dso/Abell/Abell12_600u800.md +++ b/cs/dso/Abell/Abell12_600u800.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.120285 updated_by: skybber -updated_date: 2020-09-23 20:52:19.120303 +updated_date: 2022-12-07 18:51:09.675441 --- -450x, [OIII], 6m8 +450x, [OIII], 6m8 Je třeba alespoň UHC, lepší [OIII] a střední zvětšení. s [OIII] na na okraji zářivé Mu Ori, disk PN kulatý a dobře ohraničený, tvar prstenu těžký, uprostřed jen trochu tmavší nez okraj. \ No newline at end of file diff --git a/cs/dso/Abell/Abell13.md b/cs/dso/Abell/Abell13.md index 6d50fa417..73b1dbf9d 100644 --- a/cs/dso/Abell/Abell13.md +++ b/cs/dso/Abell/Abell13.md @@ -1,6 +1,6 @@ --- name: -rating: 1 +rating: 4 references: created_by: skybber created_date: 2020-09-23 20:52:08.633035 diff --git a/cs/dso/Abell/Abell13_400u500.md b/cs/dso/Abell/Abell13_400u500.md index 69cac0b7e..ba207f7a4 100644 --- a/cs/dso/Abell/Abell13_400u500.md +++ b/cs/dso/Abell/Abell13_400u500.md @@ -4,10 +4,10 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.035747 updated_by: skybber -updated_date: 2021-02-13 09:25:30.307375 +updated_date: 2022-12-07 18:51:59.368501 --- -16" 129x, [OIII], 6m8 -občas blikající na SZ straně. Nejisté pozorování. - -**500mm** 62x - 121x, [OIII], 6m5+ +16" 129x, [OIII], 6m8 +občas blikající na SZ straně. Nejisté pozorování. + +**500mm** 62x - 121x, [OIII], 6m5+ Opět obtížné pozorování, nic z PN jako celku není vidět. 121x a [OIII] vykazuje mírné rozjasnění v místě nejjasnějšího oblouku. Problém je v tom, že v tomto bodě je skupina 15 mag hvězd, které nelze s dostatečnou jistotou ve filtru odlišit od mlhy. Pozorování spíše negativní \ No newline at end of file diff --git a/cs/dso/Abell/Abell13_600u800.md b/cs/dso/Abell/Abell13_600u800.md index 8742091f5..e162a8955 100644 --- a/cs/dso/Abell/Abell13_600u800.md +++ b/cs/dso/Abell/Abell13_600u800.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.885515 updated_by: skybber -updated_date: 2021-02-13 09:25:30.307465 +updated_date: 2022-12-07 18:51:59.368703 --- -105x, [OIII], 7m+ +105x, [OIII], 7m+ PN pouze 13'S od 66 Ori (5,6mag) , která musí být udržována mimo zorné pole, což se při použití velkých zvětšení jeví jako obtížné, proto jsou ideální okuláry s malým zorným polem. V 6,6 mm ZP zůstává PN extrémně těžká i přes vynikající vysokohorsjou oblohu a 27 "průměr. S [OIII] a se v západní časti PN jeví jako neurčitý protáhlý tvar, což odpovídá poloze nejjasnějšího oblouku. Zjasnění však nelze držet stabilně, spíše negativní. \ No newline at end of file diff --git a/cs/dso/Abell/Abell20_200u250.md b/cs/dso/Abell/Abell20_200u250.md index b27db46b8..33996fbdd 100644 --- a/cs/dso/Abell/Abell20_200u250.md +++ b/cs/dso/Abell/Abell20_200u250.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:18.912521 updated_by: skybber -updated_date: 2021-12-18 19:53:00.769066 +updated_date: 2022-12-16 16:19:23.916839 --- -47x-80x, [OIII], 6m5 + -Při 47x + [OIII] se nepřímo objeví velmi slabý povrch, který leží mezi lichoběžníkem z 14 mag hvězd. Při 80x je povrch lépe vidět a lze jej držet pouze nepřímo. Plocha zhruba kulatá bez dalších struktur. \ No newline at end of file +47x-80x, [OIII], 6m5 + +Při 47x + [OIII] se nepřímo objeví velmi slabá ploška, která leží mezi lichoběžníkem z 14 mag hvězd. Při 80x je plocha lépe vidět a lze jej držet pouze nepřímo. Tvar zhruba kulatý bez dalších struktur. \ No newline at end of file diff --git a/cs/dso/Abell/Abell20_400u500.md b/cs/dso/Abell/Abell20_400u500.md index ad1cb9403..4dbb33149 100644 --- a/cs/dso/Abell/Abell20_400u500.md +++ b/cs/dso/Abell/Abell20_400u500.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.389772 updated_by: skybber -updated_date: 2021-12-18 19:53:00.769138 +updated_date: 2022-12-16 16:19:23.916945 --- -200x, [OIII] Filtr, 6m3 -Slabě rozeznatelná již bez filtru ve zvětšení 100x. Opravdu obtížná ve 200x bez filtru, ale jistá při bočním vidění. V mlhovině a kolem ní je několik slabých hvězd. Dobře reaguje na filtry. S filtry 200x se střed jeví tmavý. Obtížný jasnější prstenec je viditelný jen asi ze 3/4, jižní čtvrtina se zdá být otevřená nebo je pod hranicí vnímání. Konce prstence 3/4 vypadají o něco jasnější než ostatní - malá zauzlení nebo hvězdy v mlhovině. +200x, [OIII] Filtr, 6m3 +Slabě rozeznatelná již bez filtru ve zvětšení 100x. Opravdu obtížná ve 200x bez filtru, ale jistá při bočním vidění. V mlhovině a kolem ní je několik slabých hvězd. Dobře reaguje na filtry. S filtry 200x se střed jeví tmavý. Obtížný jasnější prstenec je viditelný jen asi ze 3/4, jižní čtvrtina se zdá být otevřená nebo je pod hranicí vnímání. Konce prstence 3/4 vypadají o něco jasnější než ostatní - malá zauzlení nebo hvězdy v mlhovině. diff --git a/cs/dso/Abell/Abell20_600u800.md b/cs/dso/Abell/Abell20_600u800.md index 9f9076c8a..5a14ae36f 100644 --- a/cs/dso/Abell/Abell20_600u800.md +++ b/cs/dso/Abell/Abell20_600u800.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:19.470530 updated_by: skybber -updated_date: 2021-12-18 19:53:00.769188 +updated_date: 2022-12-16 16:19:23.916987 --- -172x-293x, [OIII] / UHC, 6m5 + +172x-293x, [OIII] / UHC, 6m5 + PN viditelná již bez filtru, jako výrazné zjasnění na okraji slabé hvězdné skupiny. Tušitelná centrální hvězda při 172x, nepřímo pak při 293x. Pozitivní odpověď na UHC a [OIII]. Při 4 mm pupile (172x) lze PN považovat za kulatou, dobře definovanou oblast, která se ve středu jeví trochu tmavší. S filtrem viditelná přímo. \ No newline at end of file diff --git a/cs/dso/Cr/Cr132.md b/cs/dso/Cr/Cr132.md index 05582cba0..81ac2a5b1 100644 --- a/cs/dso/Cr/Cr132.md +++ b/cs/dso/Cr/Cr132.md @@ -5,10 +5,10 @@ references: created_by: editor.cs created_date: 2020-09-23 20:52:09.095340 updated_by: skybber -updated_date: 2021-01-09 10:09:55.348535 +updated_date: 2022-12-04 09:32:50.708559 --- -![<]($IMG_DIR/dso/Cr132.png) -Otevřená hvězdokupa viditelná v dalekohledu s průměrem objektivu 8 cm jako rozsáhlé zhuštění bohatého hvězdného pola jižní části Mléčné dráhy Velkého psa. Skládá se z několika tuctů hvězd různých jasností v rozloze jeden a půl stupně. Čtyři nejjasnější hvězdy, jedna 5mag a tři 6mag vytvářejí rohy čtverce. Jak to u většiny otevřených hvězdokup s označením Collinder bývá, jsou nejlepší viditelné v triedru a v malých zvětšeních. - - - +![<]($IMG_DIR/dso/Cr132.png) +Otevřená hvězdokupa viditelná v dalekohledu s průměrem objektivu 8 cm jako rozsáhlé zhuštění bohatého hvězdného pole jižní části Mléčné dráhy Velkého psa. Skládá se z několika tuctů hvězd různých jasností v rozloze jeden a půl stupně. Čtyři nejjasnější hvězdy, jedna 5mag a tři 6mag vytvářejí rohy čtverce. Jak to u většiny otevřených hvězdokup s označením Collinder bývá, jsou nejlépe viditelné v triedru a v malých zvětšeních. + + + diff --git a/cs/dso/Jonckheere/Jonckheere320.md b/cs/dso/Jonckheere/Jonckheere320.md index 43c9faed4..a668edb77 100644 --- a/cs/dso/Jonckheere/Jonckheere320.md +++ b/cs/dso/Jonckheere/Jonckheere320.md @@ -1,10 +1,10 @@ --- name: -rating: 1 +rating: 5 references: created_by: skybber created_date: 2020-09-23 20:52:07.226889 updated_by: skybber -updated_date: 2020-09-26 20:10:52.075905 +updated_date: 2022-12-07 18:50:45.497108 --- -![<]($IMG_DIR/dso/J320.jpg) +![<]($IMG_DIR/dso/J320.jpg) diff --git a/cs/dso/Jonckheere/Jonckheere320_400u500.md b/cs/dso/Jonckheere/Jonckheere320_400u500.md index 7fbdbf440..30fc0e605 100644 --- a/cs/dso/Jonckheere/Jonckheere320_400u500.md +++ b/cs/dso/Jonckheere/Jonckheere320_400u500.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2020-09-23 20:52:18.838756 updated_by: skybber -updated_date: 2020-09-26 20:10:52.076124 +updated_date: 2022-12-07 18:50:45.497020 --- -600x, bez filtru, 6m3 +600x, bez filtru, 6m3 Ve zvětšení 66x (pupila 6mm) je velmi snadné rozpoznat jako hvězdu 9-10mag. Nejlepší pohled při 600x (pupila 0,65mm). Kolem dvou těžko rozlišitelných stelárních jader (jihovýchodní mírně jasnější) nebo uzlů, je vidět malé, ale jasné, eliptické halo, následované dalším, slabším a kulatějším vnějším halo. Filtr [OIII] má malý účinek, ale nechá více vyniknout obě jádra. Všechny hranice mlhoviny jsou velmi rozptýlené, detaily PN velmi obtížné, přestože tato neobvyklá PN je poměrně jasná. \ No newline at end of file diff --git a/cs/dso/M/M1.md b/cs/dso/M/M1.md index bf47da12d..32612cc2c 100644 --- a/cs/dso/M/M1.md +++ b/cs/dso/M/M1.md @@ -5,14 +5,14 @@ references: created_by: editor.cs created_date: 2020-09-23 20:52:06.611904 updated_by: skybber -updated_date: 2021-10-25 14:52:34.795568 +updated_date: 2022-12-03 18:41:02.389998 --- -![<]($IMG_DIR/dso/M001.jpg) -Proslulý pozůstatek po supernově, jejíž vzplanutí pozorovali 4. července roku 1054 čínští astronomové. Supernovu popsali jako červeno-bílou hvězdu s ostrými paprsky směřujícími do 4 stran. Výbuchu si všimli i američtí indiáni ze severní Arizony a díky nim se tato událost v podobě několika kreseb zachovala až do dnešních dnů. Jasností 6krát překonala Venuši a následujících 23 dní byla vidět i přes den pouhým okem. Potom postupně slábla a z oblohy se definitivně ztratila až za dalších 653 dní. Pozůstatek po supernově byl znovu nalezen až v časech objevů dalekohledů, v roce 1731 britským amatérským astronomem Johnem Bevisonem, který ji uvedl do svého hvězdného katalogu Uranographia Britannica. Podle záznamů ji nezávisle na něm objevil i Charles Messier v roce 1758 v době, kdy se k nám po 76 letech poprvé od předpovědi návratu E. Halleye vracela Halleyova kometa, pojmenována na jeho počest. Messier jistě nevěděl, že objevil jeden z nejpoutavějších a nejzvláštnějších objektů na obloze. Známý název dostala Krabí mlhovina až podle obrázku, který nakreslil v roce 1844 při pozorování svým mohutným 36 palcovým teleskopem Lord Rose v Irsku. - -Fotografie získané během jednotlivých desetiletí ukazují, že se Krabí mlhovina neustále rozšiřuje. Plynová mračna se stále rozpínají do prostoru rychlostí 1 000 km za sekundu. Je to skutečný důkaz toho, že Krabí mlhovina je opravdu pozůstatkem po supernově z roku 1054. V roce 1968 byl v jejím středu zjištěn jeden z prvních pulsarů (a později i první objevený vizuálně) - mimořádně hustá neutronová hvězda, která se kolem své osy otočí v periodě 0,033 sekundy (otočí se 33-krát za sekundu). Při každé otočce vyšle puls rádiového, X-ray a viditelného záření. Tato slabá hvězdička s označením NP0532, skutečného průměru pouze několik kilometrů, která vznikla při kolapsu jádra supernovy, nikdy nedosáhne větší než 16. hvězdnou velikost, a právě proto se pro amatérské astronomy stala skutečným "challange" objektem. Vzdálenost Krabí mlhoviny se odhaduje na 6 300 světelných let. - -I když její nesmírně složitou strukturu zahlédneme v dalekohledech s průmerem objektivu 60cm a více, stojí za to ji vyhledat, protože je to mimořádně pozoruhodný vesmírný objekt v celých dějinách astronomie a jako jediný pozůstatek po supernově v Messierovom katalogu si zaslouží speciální pozoronost. Astronomy již dlouhá léta podněcuje k výzkumu a zajímavým úvahám, navíc velmi přispěla k poznání vývoje vesmíru. Najít ji můžeme ve východní části souhvězdí, více než jeden stupeň severozápadně od ζ Tauri pod čistým, tmavým nebem i dobrým binokulárem 7 × 50 či 10 × 50 jako malý mlhavý obláček o průměru 6 × 4 obloukových minut. Dosahuje jasnost 8,4mag, takže je nepřehlédnutelná již v triedru: jeví se jako jasná oválná skvrna. Zvláštní však je, že mnoho katalogů nemá uvedenou přesnou vizuální magnitudu tohoto fascinujícího objektu. V Messier, Mallas a Kreimer určili jasnost na "8 nebo 9", Burnham uvádí "kolem 9". Jones ve své práci Messierovy mlhoviny a hvězdokupy odhadl vizuální magnitudu Krabí mlhoviny přesněji na 8,4mag. Nicméně všechny tyto odhady jsou pravděpodobně příliš slabé. - -Mlhovina je však ještě zajímavější - tvoří ji tři části: pulsar s jasností 16mag, vnitřní bublina materiálu a vnější obal hustého materiálu vyvrženého explozí supernovy. Při vysokém zvětšení je mlhovina skvrnitá - rozděluje se na tři rozdílné části táhnoucí se jihovýchodně a severozápadně. V jižní a střední části je podobná jasnost, zatímco severní část je menší a slabší. Když se fotografuje v polarizovaném světle, mlhovina odhaluje podobný trojcípý nebo zoubkovaný charakter, který indikuje existenci velmi silných magnetických polí. Zkoušel někdo pozorovat M1 velkým dalekohledem přes polarizační filtr, jaký se používá v pozemské fotografii? Východní okraj Krabí mlhoviny obsahuje nápadný zářez nebo výklenek, zesílený dlouhým filamentem směřujícím na jihovýchod. Tento filament se točí přes střední část mlhoviny na západní část, kde se rozšiřuje nad hlavní část. Sledujte pozorně a dívejte zda nezdetekujete šedý proud dotýkající se hedvábí, který separuje jižní a střední část M1. Rozšíření severního okraje jižní části zakončuje šedý proud. Vypadá to jako prodloužení mlhoviny (z východu na západ) s možnou dvojitou strukturou. - +![<]($IMG_DIR/dso/M001.jpg) +Proslulý pozůstatek po supernově, jejíž vzplanutí pozorovali 4. července roku 1054 čínští astronomové. Supernovu popsali jako červeno-bílou hvězdu s ostrými paprsky směřujícími do 4 stran. Výbuchu si všimli i američtí indiáni ze severní Arizony a díky nim se tato událost v podobě několika kreseb zachovala až do dnešních dnů. Jasností 6krát překonala Venuši a následujících 23 dní byla vidět i přes den pouhým okem. Potom postupně slábla a z oblohy se definitivně ztratila až za dalších 653 dní. Pozůstatek po supernově byl znovu nalezen až v časech objevů dalekohledů, v roce 1731 britským amatérským astronomem Johnem Bevisonem, který ji uvedl do svého hvězdného katalogu Uranographia Britannica. Podle záznamů ji nezávisle na něm objevil i Charles Messier v roce 1758 v době, kdy se k nám po 76 letech poprvé od předpovědi návratu E. Halleye vracela Halleyova kometa, pojmenována na jeho počest. Messier jistě nevěděl, že objevil jeden z nejpoutavějších a nejzvláštnějších objektů na obloze. Známý název dostala Krabí mlhovina až podle obrázku, který nakreslil v roce 1844 při pozorování svým mohutným 36 palcovým teleskopem Lord Rose v Irsku. + +Fotografie získané během jednotlivých desetiletí ukazují, že se Krabí mlhovina neustále rozšiřuje. Plynová mračna se stále rozpínají do prostoru rychlostí 1 000 km za sekundu. Je to skutečný důkaz toho, že Krabí mlhovina je opravdu pozůstatkem po supernově z roku 1054. V roce 1968 byl v jejím středu zjištěn jeden z prvních pulsarů (a později i první objevený vizuálně) - mimořádně hustá neutronová hvězda, která se kolem své osy otočí v periodě 0,033 sekundy (otočí se 33-krát za sekundu). Při každé otočce vyšle puls rádiového, X-ray a viditelného záření. Tato slabá hvězdička s označením NP0532, skutečného průměru pouze několik kilometrů, která vznikla při kolapsu jádra supernovy, nikdy nedosáhne větší než 16. hvězdnou velikost, a právě proto se pro amatérské astronomy stala skutečným "challange" objektem. Vzdálenost Krabí mlhoviny se odhaduje na 6 300 světelných let. + +I když její nesmírně složitou strukturu zahlédneme v dalekohledech s průmerem objektivu 60cm a více, stojí za to ji vyhledat, protože je to mimořádně pozoruhodný vesmírný objekt v celých dějinách astronomie a jako jediný pozůstatek po supernově v Messierovom katalogu si zaslouží speciální pozoronost. Astronomy již dlouhá léta podněcuje k výzkumu a zajímavým úvahám, navíc velmi přispěla k poznání vývoje vesmíru. Najít ji můžeme ve východní části souhvězdí, více než jeden stupeň severozápadně od ζ Tauri pod čistým, tmavým nebem i dobrým binokulárem 7 × 50 či 10 × 50 jako malý mlhavý obláček o průměru 6 × 4 obloukových minut. Dosahuje jasnost 8,4mag, takže je nepřehlédnutelná již v triedru: jeví se jako jasná oválná skvrna. Zvláštní však je, že mnoho katalogů nemá uvedenou přesnou vizuální magnitudu tohoto fascinujícího objektu. V Messier, Mallas a Kreimer určili jasnost na "8 nebo 9", Burnham uvádí "kolem 9". Jones ve své práci Messierovy mlhoviny a hvězdokupy odhadl vizuální magnitudu Krabí mlhoviny přesněji na 8,4mag. Nicméně všechny tyto odhady jsou pravděpodobně příliš slabé. + +Mlhovina je však ještě zajímavější - tvoří ji tři části: pulsar s jasností 16mag, vnitřní bublina materiálu a vnější obal hustého materiálu vyvrženého explozí supernovy. Při vysokém zvětšení je mlhovina skvrnitá - rozděluje se na tři rozdílné části táhnoucí se jihovýchodně a severozápadně. V jižní a střední části je podobná jasnost, zatímco severní část je menší a slabší. Když se fotografuje v polarizovaném světle, mlhovina odhaluje podobný trojcípý nebo zoubkovaný charakter, který indikuje existenci velmi silných magnetických polí. Zkoušel někdo pozorovat M1 velkým dalekohledem přes polarizační filtr, jaký se používá v pozemské fotografii? Východní okraj Krabí mlhoviny obsahuje nápadný zářez nebo výklenek, zesílený dlouhým filamentem směřujícím na jihovýchod. Tento filament se točí přes střední část mlhoviny na západní část, kde se rozšiřuje nad hlavní část. Sledujte pozorně a dívejte zda nezdetekujete šedý proud dotýkající se hedvábí, který separuje jižní a střední část M1. Rozšíření severního okraje jižní části zakončuje šedý proud. Vypadá to jako prodloužení mlhoviny (z východu na západ) s možnou dvojitou strukturou. + diff --git a/cs/dso/M/M1_200u250.md b/cs/dso/M/M1_200u250.md index ff94caf6b..79a77d2aa 100644 --- a/cs/dso/M/M1_200u250.md +++ b/cs/dso/M/M1_200u250.md @@ -3,7 +3,7 @@ aperture: 200/250 rating: 5 created_by: skybber created_date: 2020-09-23 20:52:16.742231 -updated_by: danielkurtin@seznam.cz -updated_date: 2021-01-29 12:56:42.704747 +updated_by: skybber +updated_date: 2022-12-03 18:41:02.389822 --- Potěšující pohled poskytuje dalekohled až od průměru 150 mm a zvětšení kolem 125x. Mlhovinový filtr trošku pomůže, ale nerozvine objekt tak dobře jako nějakou planetárku či emisní mlhovinu. V dalekohledu s průměrem objektivu 200 mm se ukáže jako mlhavá, šedobílá oválná plocha, která pěkně kontrastuje s na hvězdy bohatým okolím. \ No newline at end of file diff --git a/cs/dso/M/M1_300u350.md b/cs/dso/M/M1_300u350.md index e7b456c7c..e69d28084 100644 --- a/cs/dso/M/M1_300u350.md +++ b/cs/dso/M/M1_300u350.md @@ -4,6 +4,6 @@ rating: 5 created_by: skybber created_date: 2020-09-23 20:52:16.843114 updated_by: skybber -updated_date: 2020-09-23 20:52:16.843139 +updated_date: 2022-12-03 18:41:02.389875 --- Při pozornějším pohledu jsou v poměrně jasné mlhavé skvrně nějaké slabší skvrnky a nerovná zjasnění. \ No newline at end of file diff --git a/cs/dso/M/M1_400u500.md b/cs/dso/M/M1_400u500.md index db41f469d..cc70b07ba 100644 --- a/cs/dso/M/M1_400u500.md +++ b/cs/dso/M/M1_400u500.md @@ -4,6 +4,6 @@ rating: 5 created_by: skybber created_date: 2020-09-23 20:52:16.222121 updated_by: skybber -updated_date: 2020-09-23 20:52:16.222156 +updated_date: 2022-12-03 18:41:02.389914 --- Mlhovina má nepravidelný okraj . Během vynikající noci můžeme spatřit bočním pohledem nerovné plošné zjasnění a náznaky vláknitých detailů. Jihovýchodní rozhraní je mnohem slabší, protože se tam noří tmavý záliv, severovýchodní rozhraní obsahuje naopak nezřetelný zářez. \ No newline at end of file diff --git a/cs/dso/M/M1_600u800.md b/cs/dso/M/M1_600u800.md index ae982ddab..379674c42 100644 --- a/cs/dso/M/M1_600u800.md +++ b/cs/dso/M/M1_600u800.md @@ -4,6 +4,6 @@ rating: 5 created_by: skybber created_date: 2020-09-23 20:52:17.644297 updated_by: skybber -updated_date: 2020-09-23 20:52:17.644316 +updated_date: 2022-12-03 18:41:02.389950 --- -Skutečným vizuální zážitkem se stává pohled na Krabí mlhovinu v dalekohledech těch největších průměrů. Obrazu v dalekohledu o průměru 70-90cm, při použití OIII filtru, naprosto dominuje vláknitá struktura, která pokrývá celou mlhovinu. Úplně uprostřed je možné zahlédnout dokonce i pulzar. Komplex M1 ve velkém dobsnu je jedním z vůbec nejpůsobivějších vizuálních zážitků, které může obloha nabídnout. \ No newline at end of file +Skutečným vizuální zážitkem se stává pohled na Krabí mlhovinu v dalekohledech těch největších průměrů. Obrazu v dalekohledu o průměru 70-90cm, při použití OIII filtru, naprosto dominuje vláknitá struktura, která pokrývá celou mlhovinu. Úplně uprostřed je možné zahlédnout dokonce i pulzar. Komplex M1 ve velkém dobsonu je jedním z vůbec nejpůsobivějších vizuálních zážitků, které může obloha nabídnout. \ No newline at end of file diff --git a/cs/dso/M/M45.md b/cs/dso/M/M45.md index cc7ab3ba9..e2270e78e 100644 --- a/cs/dso/M/M45.md +++ b/cs/dso/M/M45.md @@ -5,12 +5,12 @@ references: created_by: editor.cs created_date: 2020-09-23 20:52:06.143559 updated_by: skybber -updated_date: 2021-10-25 14:47:20.627905 +updated_date: 2022-12-03 18:31:30.250070 --- -Otevřená hvězdokupa známá také pod názvem "Kuřátka" či "Sedm nebeských sester". Možná nejkrásnější otevřená hvězdokupa na celé obloze - je jedno zda se na ni díváme pouhým okem, triedrem či dalekohledem. I během průměrných pozorovacích podmínek ve městech při úplňku Měsíce bychom měli v Plejádách na první pohled pouhým okem rozlišit šest hvězd. Nejjasnější z nich je modrobílý obr Alcyone (η Tau - 2,87mag), potom následuje Atlas (27 Tau - 3,63mag), Electra (17 Tau - 3,7mag), Maia (20 Tau - 3,87mag), Merope ( 23 Tau - 4,18mag) a taygeta (19 Tau - 4,3 m). Pokud se naskytne tmavá průzračná noc, měli bychom bez problémů spatřit ještě Pleione (28 Tau - 5,9mag), Celaeno (16 Tau - 5,46mag) a Sterope I (21 Tau - 5,76mag). V závislosti na bystrosti zraku a atmosférických podmínkách je v dosahu ještě dalších sedm hvězd, přičemž z odlehlých končin bychom jich mohli napočítat až kolem 20. Devět nejjasnějších hvězd je soustředěno na ploše jednoho stupně, ale další hvězdy skupiny můžeme najít ještě o stupeň dál. Vhodné je pozorovat triedrem případně dalekohledem, přičemž je třeba použít okulár s velmi malým zvětšením a širokým zorným polem, abychom zahlédli celou skupinu. Odhaduje se, že celkově hvězdokupa obsahuje 400-500 hvězd, přičemž 200 z nich můžeme rozpoznat středním amatérským dalekohledem. - -Plejády, se středem vzdáleným asi 444 světelných let, jsou čtvrtou nejbližší otevřenou hvězdokupou k naší Sluneční soustavě. Její nejjasnější hvězdy jsou všechny mladí, horcí, modrobílý obři absolutní magnitudy od -1,5 po -2,5 (červení obři zcela chybí, ale naopak byli objeveni hnědí trpaslíci s malou hmotností). Tak například nejjasnější hvězda Alcyone zdánlivé jasnosti 2,87mag má absolutní magnitudu -2,7. Prach, který tak esteticky odráží modré světlo těchto hvězd, ve skutečnosti s hvězdokupou vůbec nesouvisí. Plejády jsou staré 100 milionů let a vykazují dlouhý pohyb směřující ven z mezihvězdného plynu a prachu, ze kterého byly zrozené. V současnosti procházejí okrajem tmavě prachového komplexu v Býku. Není náhoda, že na barevných fotografiích reflexní mlhoviny vypadají modré jako samotné hvězdy. Modré světlo je rozptylované lépe než červené, proto je záře hvězd Plejád na prachu reflexní mlhoviny dobře vidět. - -Nejjasnější členové kupy ve tvaru jakési "naběračky" dominují pozadí slabších hvězd už v triedru nebo malém dalekohledu. Kupa obsahuje řadu atraktivních dvojhvězd. Zvláštní řetězec hvězd 7-8mag začíná u dvojhvězdě Struve 450 a pokračuje hned jižně k hvězdě Alcyone a východně k hvězdě Merope, pak směřuje nejprve jižně a potom jihovýchodně. Alcyone má ve svém bezprostředním sousedství tři slabší hvězdy, čímž vytváří pěknou čtyřhvězdu. Atlas vytváří s Pleione širokou dvojhvězdu. Další známou je Asterope - nebo Sterope I a Sterope II, kterou volné oko sice nerozliší, ale už triedr ji zobrazí jako široký pár. Reflexní mlhoviny zahalující hvězdy "naběračky" jsou nejjasnější a nejsnáze pozorovatelné kolem hvězdy Merope, kde mají i označení **NGC 1435 (Tempel nebula)**. Kolem této hvězdy se během vynikajících pozorovacích podmínek mohou blýsknout už v triedru 10 × 50. Mlhovina vypadá jako světlá šmouha, která se táhne do vzdálenosti asi deseti úhlových minut a mírně vystupuje nad jas okolní oblohy. V dalekohledu s průměrem objektivu kolem 200mm a při malém zvětšení můžeme odhalit slabý závoj mlhoviny kolem dalších dvou z jasnějších hvězd. Přestože se jedná o reflexní mlhoviny, tak pomůže i filtr O-III, i když pravda, že zastíní její slabší vnější části. - -Myzer: Malou inspiraci možná najdete v následujících řádcích, z jednoho pozorování koncem léta během velmi kvalitních podmínek: Hodinu před koncem astronomické noci jsem se rozhodl zjistit, kolik hvězd asi uvidím pouhým okem v Plejádách, které se již nacházely dost vysoko nad obzorem (50 stupňů ). Není to sice mým zvykem, ale tentokrát jsem udělal výjimku a začal všechno zakreslovat. Na papír jsem přenesl šest hlavních nejjasnějších hvězd nápadné hvězdokupy (Alcyone, Merope, Atlas, Maia, Electra, taygeta) a začal se konečně soustředěně dívat. Dalších pět hvězd (Pleione, CELEANO, Asterope, 18 Tau, HD 23753) bylo celkem lehkých, protože nejslabší z nich má 5,76mag. Ostatní hvězdy přibývaly už jen postupně, protože nebyly vidět stabilně a pouze občas problikávaly. Proto jsem jim věnoval hodně času, s cílem zakreslit je na správném místě a vyhnout se chybám. Výsledek byl více než nečekaný - napočítal jsem až sedmnáct hvězd! Zkouška správnosti však následovala až o den později, když jsem si náčrt porovnával s programem Sky Charts. Vše bylo zpečetěno, poloha hvězd jednoznačně seděla se skutečností. Nejslabší zachycena hvězda (SAO 76264) má vizuální jasnost 6,96mag. Shodou okolností je to i hvězda s nízkým barevným indexem spektrálního typu A, tedy velmi vhodná pro určování MHV. +Otevřená hvězdokupa známá také pod názvem "Kuřátka" či "Sedm nebeských sester". Možná nejkrásnější otevřená hvězdokupa na celé obloze - je jedno zda se na ni díváme pouhým okem, triedrem či dalekohledem. I během průměrných pozorovacích podmínek ve městech při úplňku Měsíce bychom měli v Plejádách na první pohled pouhým okem rozlišit šest hvězd. Nejjasnější z nich je modrobílý obr Alcyone (η Tau - 2,87mag), potom následuje Atlas (27 Tau - 3,63mag), Electra (17 Tau - 3,7mag), Maia (20 Tau - 3,87mag), Merope ( 23 Tau - 4,18mag) a taygeta (19 Tau - 4,3 m). Pokud se naskytne tmavá průzračná noc, měli bychom bez problémů spatřit ještě Pleione (28 Tau - 5,9mag), Celaeno (16 Tau - 5,46mag) a Sterope I (21 Tau - 5,76mag). V závislosti na bystrosti zraku a atmosférických podmínkách je v dosahu ještě dalších sedm hvězd, přičemž z odlehlých končin bychom jich mohli napočítat až kolem 20. Devět nejjasnějších hvězd je soustředěno na ploše jednoho stupně, ale další hvězdy skupiny můžeme najít ještě o stupeň dál. Vhodné je pozorovat triedrem případně dalekohledem, přičemž je třeba použít okulár s velmi malým zvětšením a širokým zorným polem, abychom zahlédli celou skupinu. Odhaduje se, že celkově hvězdokupa obsahuje 400-500 hvězd, přičemž 200 z nich můžeme rozpoznat středním amatérským dalekohledem. + +Plejády, se středem vzdáleným asi 444 světelných let, jsou čtvrtou nejbližší otevřenou hvězdokupou k naší Sluneční soustavě. Její nejjasnější hvězdy jsou všechny mladí, horcí, modrobílí obři absolutní magnitudy od -1,5 po -2,5 (červení obři zcela chybí, ale naopak byli objeveni hnědí trpaslíci s malou hmotností). Tak například nejjasnější hvězda Alcyone zdánlivé jasnosti 2,87mag má absolutní magnitudu -2,7. Prach, který tak esteticky odráží modré světlo těchto hvězd, ve skutečnosti s hvězdokupou vůbec nesouvisí. Plejády jsou staré 100 milionů let a vykazují dlouhý pohyb směřující ven z mezihvězdného plynu a prachu, ze kterého byly zrozené. V současnosti procházejí okrajem temného prachového komplexu v Býku. Není náhoda, že na barevných fotografiích reflexní mlhoviny vypadají modré jako samotné hvězdy. Modré světlo je rozptylované lépe než červené, proto je záře hvězd Plejád na prachu reflexní mlhoviny dobře vidět. + +Nejjasnější členové kupy ve tvaru jakési "naběračky" dominují pozadí slabších hvězd už v triedru nebo malém dalekohledu. Kupa obsahuje řadu atraktivních dvojhvězd. Zvláštní řetězec hvězd 7-8mag začíná u dvojhvězdě Struve 450 a pokračuje hned jižně k hvězdě Alcyone a východně k hvězdě Merope, pak směřuje nejprve jižně a potom jihovýchodně. Alcyone má ve svém bezprostředním sousedství tři slabší hvězdy, čímž vytváří pěknou čtyřhvězdu. Atlas vytváří s Pleione širokou dvojhvězdu. Další známou je Asterope - nebo Sterope I a Sterope II, kterou volné oko sice nerozliší, ale už triedr ji zobrazí jako široký pár. Reflexní mlhoviny zahalující hvězdy "naběračky" jsou nejjasnější a nejsnáze pozorovatelné kolem hvězdy Merope, kde mají i označení **NGC 1435 (Tempel nebula)**. Kolem této hvězdy se během vynikajících pozorovacích podmínek mohou blýsknout už v triedru 10 × 50. Mlhovina vypadá jako světlá šmouha, která se táhne do vzdálenosti asi deseti úhlových minut a mírně vystupuje nad jas okolní oblohy. V dalekohledu s průměrem objektivu kolem 200mm a při malém zvětšení můžeme odhalit slabý závoj mlhoviny kolem dalších dvou z jasnějších hvězd. Přestože se jedná o reflexní mlhoviny, tak pomůže i filtr O-III, i když pravda, že zastíní její slabší vnější části. + +Myzer: Malou inspiraci možná najdete v následujících řádcích, z jednoho pozorování koncem léta během velmi kvalitních podmínek: Hodinu před koncem astronomické noci jsem se rozhodl zjistit, kolik hvězd asi uvidím pouhým okem v Plejádách, které se již nacházely dost vysoko nad obzorem (50 stupňů ). Není to sice mým zvykem, ale tentokrát jsem udělal výjimku a začal všechno zakreslovat. Na papír jsem přenesl šest hlavních nejjasnějších hvězd nápadné hvězdokupy (Alcyone, Merope, Atlas, Maia, Electra, taygeta) a začal se konečně soustředěně dívat. Dalších pět hvězd (Pleione, CELEANO, Asterope, 18 Tau, HD 23753) bylo celkem lehkých, protože nejslabší z nich má 5,76mag. Ostatní hvězdy přibývaly už jen postupně, protože nebyly vidět stabilně a pouze občas problikávaly. Proto jsem jim věnoval hodně času, s cílem zakreslit je na správném místě a vyhnout se chybám. Výsledek byl více než nečekaný - napočítal jsem až sedmnáct hvězd! Zkouška správnosti však následovala až o den později, když jsem si náčrt porovnával s programem Sky Charts. Vše bylo zpečetěno, poloha hvězd jednoznačně seděla se skutečností. Nejslabší zachycena hvězda (SAO 76264) má vizuální jasnost 6,96mag. Shodou okolností je to i hvězda s nízkým barevným indexem spektrálního typu A, tedy velmi vhodná pro určování MHV. diff --git a/cs/dso/NGC/1400-1500/NGC1409.md b/cs/dso/NGC/1400-1500/NGC1409.md new file mode 100644 index 000000000..21cf731d0 --- /dev/null +++ b/cs/dso/NGC/1400-1500/NGC1409.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-03 19:09:41.026182 +updated_by: +updated_date: 2022-12-03 12:58:17.769452 +--- diff --git a/cs/dso/NGC/1400-1500/NGC1409_400u500.md b/cs/dso/NGC/1400-1500/NGC1409_400u500.md new file mode 100644 index 000000000..aef45a4a1 --- /dev/null +++ b/cs/dso/NGC/1400-1500/NGC1409_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-03 19:09:41.028907 +updated_by: skybber +updated_date: 2022-12-03 19:09:41.029920 +--- +slabá, malá, oválná JJZ-SSV. Jedná se o kontaktní pár s NGC 1410 - jen 14" mezi středy. Při vysokém zvětšení se jeví slabá, malá, kulatá, malé jasné jádro. NGC 1410 je jen 15" SV ve společném halo. Nachází se na hranici Eridanu. \ No newline at end of file diff --git a/cs/dso/NGC/1500-1600/NGC1555.md b/cs/dso/NGC/1500-1600/NGC1555.md new file mode 100644 index 000000000..dc725d3fd --- /dev/null +++ b/cs/dso/NGC/1500-1600/NGC1555.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-03 20:09:07.416809 +updated_by: +updated_date: 2022-12-03 18:39:04.039392 +--- diff --git a/cs/dso/NGC/1500-1600/NGC1555_400u500.md b/cs/dso/NGC/1500-1600/NGC1555_400u500.md new file mode 100644 index 000000000..7ed28cc2a --- /dev/null +++ b/cs/dso/NGC/1500-1600/NGC1555_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-03 20:09:07.419504 +updated_by: skybber +updated_date: 2022-12-03 20:11:38.418182 +--- +(11/10/96): Hindova proměnná (reflexní) mlhovina, osvětlená hvězdou T Tauri (9-13). Při zvětšení 100x a 140x (bez filtru) byl velmi podezřelý extrémně slabý zákal na západní nebo ZJZ straně T Tauri (9. mag) ve směru hvězdy 14. mag západně nebo mírně jižně (tato hvězda je v poloze NGC 1554 = "Struveho ztracená mlhovina"). Při zvětšení 100x nebyly v mlhovině vidět žádné detaily (nevypadala jako oblouk), ale náčrtek pořízený při zvětšení 100x přesně odpovídal orientaci mlhoviny vzhledem k T Tauri. Při zvětšení 220x nebyla mlhovina viditelná a za T Tauri nebyla zaznamenána žádná mlhovina. \ No newline at end of file diff --git a/cs/dso/NGC/1500-1600/NGC1555_600u800.md b/cs/dso/NGC/1500-1600/NGC1555_600u800.md new file mode 100644 index 000000000..894763bc4 --- /dev/null +++ b/cs/dso/NGC/1500-1600/NGC1555_600u800.md @@ -0,0 +1,9 @@ +--- +aperture: 600/800 +rating: 1 +created_by: skybber +created_date: 2022-12-03 20:11:38.417429 +updated_by: skybber +updated_date: 2022-12-03 20:11:38.418288 +--- +(1/12/13): 200x, bez filtru, byla Hindova proměnná mlhovina ihned vidět jako velmi slabá, poměrně malá, protáhlá mlhovina, dlouhá zhruba 40" a mírně zakřivená nebo vykloněná k západu. Proměnná reflexní mlhovina se zdála být nerovnoměrně osvětlená, i když byla příliš slabá na to, abychom viděli nějaké konkrétní detaily. Tuto známou mlhovinu osvětluje T Tauri (10-10,5 mag), jen 35" východně. T Tauri je dokonale kolineární s hvězdou HD 27560 8,4 mag 5,6' JZ a hvězdou 12 mag 4,7' JZ. Mlhovina se pravděpodobně zjasnila od pozorování v roce 1996 mým 17,5" přístrojem. \ No newline at end of file diff --git a/cs/dso/NGC/1500-1600/NGC1555_900u1200.md b/cs/dso/NGC/1500-1600/NGC1555_900u1200.md new file mode 100644 index 000000000..e8112d973 --- /dev/null +++ b/cs/dso/NGC/1500-1600/NGC1555_900u1200.md @@ -0,0 +1,9 @@ +--- +aperture: 900/1200 +rating: 1 +created_by: skybber +created_date: 2022-12-03 20:11:38.417811 +updated_by: skybber +updated_date: 2022-12-03 20:11:38.418344 +--- + (10/29/19): při 375x byla tato proměnná mlhovina okamžitě spatřena jako rozptýlená, protáhlá skvrna západně od T Tauri. Dalekohled se však ve větru třásl a viditelnost byla špatná, takže chyběly detaily. \ No newline at end of file diff --git a/cs/dso/NGC/1500-1600/NGC1587.md b/cs/dso/NGC/1500-1600/NGC1587.md new file mode 100644 index 000000000..598d368fc --- /dev/null +++ b/cs/dso/NGC/1500-1600/NGC1587.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-03 19:07:30.947322 +updated_by: +updated_date: 2022-12-03 18:39:04.039392 +--- diff --git a/cs/dso/NGC/1500-1600/NGC1587_300u350.md b/cs/dso/NGC/1500-1600/NGC1587_300u350.md new file mode 100644 index 000000000..ba5f2b52d --- /dev/null +++ b/cs/dso/NGC/1500-1600/NGC1587_300u350.md @@ -0,0 +1,9 @@ +--- +aperture: 300/350 +rating: 1 +created_by: skybber +created_date: 2022-12-03 19:07:30.949738 +updated_by: skybber +updated_date: 2022-12-03 19:08:24.274133 +--- +středně světlá, malá, téměř kulatá, malé světlé jádro. Tvoří dvojici s NGC 1588 1' V. NGC 1589 leží 12' S. Nachází se uprostřed mezi 44 a 45 Tauri. \ No newline at end of file diff --git a/cs/dso/NGC/1500-1600/NGC1587_400u500.md b/cs/dso/NGC/1500-1600/NGC1587_400u500.md new file mode 100644 index 000000000..3193fb2b8 --- /dev/null +++ b/cs/dso/NGC/1500-1600/NGC1587_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-03 19:08:24.272641 +updated_by: skybber +updated_date: 2022-12-03 19:08:24.274242 +--- +poměrně jasná, středně velká, mírně protáhlá JZ-SV, 1,2'x1,0', dobře koncentrovaná s velmi jasným jádrem a hvězdným jádérkem. Tvoří těsný pár s NGC 1588 0,9' V. V trojici s NGC 1589 12' N. NGC 1587 je nejjasnějším členem skupiny galaxií LGG 117 (z = .012). \ No newline at end of file diff --git a/cs/dso/NGC/1700-1800/NGC1750.md b/cs/dso/NGC/1700-1800/NGC1750.md new file mode 100644 index 000000000..9b0c1b6a1 --- /dev/null +++ b/cs/dso/NGC/1700-1800/NGC1750.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-03 20:25:56.700028 +updated_by: +updated_date: 2022-12-03 18:39:04.039392 +--- diff --git a/cs/dso/NGC/1700-1800/NGC1750_400u500.md b/cs/dso/NGC/1700-1800/NGC1750_400u500.md new file mode 100644 index 000000000..b2ea7bb7f --- /dev/null +++ b/cs/dso/NGC/1700-1800/NGC1750_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-03 20:25:56.707977 +updated_by: skybber +updated_date: 2022-12-03 20:25:56.714354 +--- +nápadná podskupina dvou desítek hvězd uvnitř NGC 1746 na JZ straně. Poměrně velký oválný obrys orientovaný SZ-JV, uprostřed prázdný. Obsahuje pěknou dvojhvězdu 9,1/9,1 ve 20". NGC 1758 je blízko SV (i když s ní pravděpodobně fyzicky nesouvisí). Moderní katalogy vztahují NGC 1746 k celé hvězdokupě (viz popis), ačkoli NGC 1750 (od Williama Herschela) a NGC 1746 (od d'Arresta) jsou buď totožné, nebo jen části téže hvězdokupy. \ No newline at end of file diff --git a/cs/dso/NGC/1800-1900/NGC1819.md b/cs/dso/NGC/1800-1900/NGC1819.md new file mode 100644 index 000000000..4cbc0d643 --- /dev/null +++ b/cs/dso/NGC/1800-1900/NGC1819.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-07 18:47:45.253533 +updated_by: +updated_date: 2022-12-05 00:11:59.873325 +--- diff --git a/cs/dso/NGC/1800-1900/NGC1819_300u350.md b/cs/dso/NGC/1800-1900/NGC1819_300u350.md new file mode 100644 index 000000000..5dce463d3 --- /dev/null +++ b/cs/dso/NGC/1800-1900/NGC1819_300u350.md @@ -0,0 +1,9 @@ +--- +aperture: 300/350 +rating: 1 +created_by: skybber +created_date: 2022-12-07 18:47:45.255393 +updated_by: skybber +updated_date: 2022-12-07 18:47:45.256538 +--- + slabá, velmi malá, jasné jádro, protáhlá SZ-JV. Nachází se 12,5' J od SAO 112508 mag 8. \ No newline at end of file diff --git a/cs/dso/NGC/1900-2000/NGC1973.md b/cs/dso/NGC/1900-2000/NGC1973.md index 3c77d015d..603f321eb 100644 --- a/cs/dso/NGC/1900-2000/NGC1973.md +++ b/cs/dso/NGC/1900-2000/NGC1973.md @@ -5,7 +5,7 @@ references: created_by: editor.cs created_date: 2020-09-23 20:52:05.671530 updated_by: skybber -updated_date: 2020-09-28 12:09:28.229277 +updated_date: 2022-12-07 17:52:56.075572 --- -![<]($IMG_DIR/dso/NGC1973.jpg) -Poměrně jasný mlhovinový komplex mezi M42 na jihu a otevřenou hvězdokupou NGC 1981 na severu. Blízkost mlhoviny k M42 ji činí druhořadou, ale jinak je to zajímavý objekt, který si zaslouží pozornost. Tyto tři mlhoviny jsou slabší ostvětlenými částmi téhož velkého oblaku plynu a prachu. NGC 1977 je ze všech největší, ale je ji nejtěžší vidět, kvůli záři 42 Ori (4,7mag). \ No newline at end of file +![<]($IMG_DIR/dso/NGC1973.jpg) +Poměrně jasný mlhovinový komplex mezi M42 na jihu a otevřenou hvězdokupou NGC 1981 na severu. Blízkost mlhoviny k M42 ji činí druhořadou, ale jinak je to zajímavý objekt, který si zaslouží pozornost. Tyto tři mlhoviny jsou slabší ostvětlenými částmi téhož velkého oblaku plynu a prachu. NGC 1977 je ze všech největší, ale je ji nejhůře vidět, kvůli záři 42 Ori (4,7mag). \ No newline at end of file diff --git a/cs/dso/NGC/1900-2000/NGC1973_300u350.md b/cs/dso/NGC/1900-2000/NGC1973_300u350.md index dd77ad7fb..dbbae668f 100644 --- a/cs/dso/NGC/1900-2000/NGC1973_300u350.md +++ b/cs/dso/NGC/1900-2000/NGC1973_300u350.md @@ -4,6 +4,6 @@ rating: created_by: editor.cs created_date: 2020-09-23 20:52:15.577255 updated_by: skybber -updated_date: 2020-09-28 12:09:28.229441 +updated_date: 2022-12-07 17:54:52.642184 --- -75x: Je velkým matným půlkruhem vyhloubeným na jih. NGC 1973, hned severně od NGC 1977, je poměrně zřejmým, matným 5'x3'zväzkom, prodlouženým V-Z. NGC 1975 je mnohem menší skvrnou ležící hned severovýchodně od NGC 1973. Oblast je pokropená velmi slabými mlhavými viry. \ No newline at end of file +75x: Je velkým matným půlkruhem vyhloubeným na jih. NGC 1973, hned severně od NGC 1977, je poměrně zřejmým, matným 5'x3' svazkem, prodlouženým V-Z. NGC 1975 je mnohem menší skvrnou ležící hned severovýchodně od NGC 1973. Celá oblast je pokrytá velmi slabým mlhavým závojem. \ No newline at end of file diff --git a/cs/dso/NGC/2000-2100/NGC2071.md b/cs/dso/NGC/2000-2100/NGC2071.md index 1f8d9aeb2..7986a9d22 100644 --- a/cs/dso/NGC/2000-2100/NGC2071.md +++ b/cs/dso/NGC/2000-2100/NGC2071.md @@ -1,6 +1,6 @@ --- name: -rating: 1 +rating: 5 references: created_by: skybber created_date: 2022-02-15 18:44:14.381782 diff --git a/cs/dso/NGC/2000-2100/NGC2071_200u250.md b/cs/dso/NGC/2000-2100/NGC2071_200u250.md index d6bd9f962..6412c90ed 100644 --- a/cs/dso/NGC/2000-2100/NGC2071_200u250.md +++ b/cs/dso/NGC/2000-2100/NGC2071_200u250.md @@ -4,6 +4,6 @@ rating: 1 created_by: skybber created_date: 2022-02-15 18:44:14.669193 updated_by: skybber -updated_date: 2022-02-15 18:44:14.927603 +updated_date: 2022-12-07 18:50:32.398233 --- -slabá reflexní mlhovina. Nachází se 15' SZ od M78 . Obklopuje jihovýchodní člen dvojhvězdy 10. mag. +slabá reflexní mlhovina. Nachází se 15' SZ od M78 . Obklopuje jihovýchodní člen dvojhvězdy 10. mag. diff --git a/cs/dso/NGC/2000-2100/NGC2071_400u500.md b/cs/dso/NGC/2000-2100/NGC2071_400u500.md index ece902c4c..b35282615 100644 --- a/cs/dso/NGC/2000-2100/NGC2071_400u500.md +++ b/cs/dso/NGC/2000-2100/NGC2071_400u500.md @@ -4,8 +4,8 @@ rating: 1 created_by: skybber created_date: 2022-02-15 18:44:14.788725 updated_by: skybber -updated_date: 2022-02-15 18:44:14.927750 +updated_date: 2022-12-07 18:50:32.398330 --- -poměrně jasná reflexní mlhovina obklopující hvězdu 9,5 mag, průměr 3,5'. Tvar se zdá být nepravidelný (i když bez zřetelných hranic), ale zasahuje spíše na jižní stranu hvězdy, která má slabého průvodce blízko jihu. Druhá hvězda 9,5 mag (nezúčastněná) leží 3,5' SZ. V poli podivně chybí hvězdy, které jsou cloněné mlhovinou. - +poměrně jasná reflexní mlhovina obklopující hvězdu 9,5 mag, průměr 3,5'. Tvar se zdá být nepravidelný (i když bez zřetelných hranic), ale zasahuje spíše na jižní stranu hvězdy, která má slabého průvodce blízko jihu. Druhá hvězda 9,5 mag (nezúčastněná) leží 3,5' SZ. V poli podivně chybí hvězdy, které jsou cloněné mlhovinou. + 17,5": Poměrně jasná reflexní mlhovina obklopuje hvězdu 10. mag, i když zasahuje dále na jih. Druhá hvězda 13. mag je zakotvena jižně od jasné hvězdy. Kruhový obrys postupně mizí v pozadí. Hvězda 10. mag. je 3,5' SZ, ale pole je kupodivu bez hvězd kvůli zakrývajícímu prachu. Nachází se 15' SZ od M78 . \ No newline at end of file diff --git a/cs/dso/NGC/2100-2200/IC2162.md b/cs/dso/NGC/2100-2200/IC2162.md index 4bdd5bf8c..f00a29d2f 100644 --- a/cs/dso/NGC/2100-2200/IC2162.md +++ b/cs/dso/NGC/2100-2200/IC2162.md @@ -1,6 +1,6 @@ --- name: -rating: 1 +rating: 5 references: created_by: skybber created_date: 2022-02-15 18:39:57.816816 diff --git a/cs/dso/NGC/2100-2200/IC2162_400u500.md b/cs/dso/NGC/2100-2200/IC2162_400u500.md index e81015471..0ef056d7b 100644 --- a/cs/dso/NGC/2100-2200/IC2162_400u500.md +++ b/cs/dso/NGC/2100-2200/IC2162_400u500.md @@ -4,6 +4,6 @@ rating: 1 created_by: skybber created_date: 2022-02-15 18:39:58.178083 updated_by: skybber -updated_date: 2022-02-15 18:39:58.342149 +updated_date: 2022-12-07 18:48:15.089632 --- -při zvětšení 100x bez filtru byla IC 2162 viditelná jako sousedící dvě slabé kruhové záře obklopující hvězdy 10,5-11 mag. IC 2162 = Sh 2-255 je jasnější a větší z dvojice, má průměr téměř 4' a je poměrně symetrická. Necelých 5' západně od ní se nachází samostatná slabší záře o průměru 3' (Sh 2-257). Tato dvojice uzlů s nízkou excitací záření se nachází uprostřed mezi dvěma hvězdami 6. mag s rozestupem 50' poblíž okraje pole. Nedaleko jihozápadně od Sh 2-257 se nachází velmi slabá skvrna mlhoviny Sh 2-256, která však nebyla vizuálně pozorována, stejně jako větší HII oblast Sh 2-254, záře s nízkou povrchovou jasností západně od ní (průměr 11'). +při zvětšení 100x bez filtru byla IC 2162 viditelná jako sousedící dvě slabé kruhové záře obklopující hvězdy 10,5-11 mag. IC 2162 = Sh 2-255 je jasnější a větší z dvojice, má průměr téměř 4' a je poměrně symetrická. Necelých 5' západně od ní se nachází samostatná slabší záře o průměru 3' (Sh 2-257). Tato dvojice uzlů s nízkou excitací záření se nachází uprostřed mezi dvěma hvězdami 6. mag s rozestupem 50' poblíž okraje pole. Nedaleko jihozápadně od Sh 2-257 se nachází velmi slabá skvrna mlhoviny Sh 2-256, která však nebyla vizuálně pozorována, stejně jako větší HII oblast Sh 2-254, záře s nízkou povrchovou jasností západně od ní (průměr 11'). diff --git a/cs/dso/NGC/2100-2200/IC2162_600u800.md b/cs/dso/NGC/2100-2200/IC2162_600u800.md index 140a41827..757fa7100 100644 --- a/cs/dso/NGC/2100-2200/IC2162_600u800.md +++ b/cs/dso/NGC/2100-2200/IC2162_600u800.md @@ -4,6 +4,6 @@ rating: 1 created_by: skybber created_date: 2022-02-15 18:39:58.262216 updated_by: skybber -updated_date: 2022-02-15 18:39:58.342274 +updated_date: 2022-12-07 18:48:15.089773 --- IC 2162 = Sh 2-255 je nejjasnější a nejvýchodnější ze čtyř kruhových nízkoexcitačních emisních mlhovin, přičemž Sh 2-257 a Sh 2-254 jsou seřazeny zhruba na západě. Při použití zvětšení 125x (21mm Ethos) a filtru H-beta se jevila jako středně jasná kruhová záře o průměru ~3,5', obklopující excitační hvězdu mag 11,6. Záře se jeví jako velmi jasná, kulatá, s průměrem ~3,5'. Sh 2-257 leží 5' západně a má podobnou velikost, ale obklopuje několik hvězd a má nižší povrchovou jasnost.Sh 2-256 má podobnou velikost, ale obklopuje několik hvězd a má nižší povrchovou jasnost. \ No newline at end of file diff --git a/cs/dso/NGC/2100-2200/IC2177.md b/cs/dso/NGC/2100-2200/IC2177.md index faa669f92..e23d1093d 100644 --- a/cs/dso/NGC/2100-2200/IC2177.md +++ b/cs/dso/NGC/2100-2200/IC2177.md @@ -5,6 +5,6 @@ references: created_by: editor.cs created_date: 2020-09-23 20:52:04.541620 updated_by: skybber -updated_date: 2020-11-15 17:04:55.876238 +updated_date: 2023-01-07 14:35:30.152486 --- -![<]($IMG_DIR/dso/Sh2-292.jpg) +![<]($IMG_DIR/dso/IC2177.jpg) diff --git a/cs/dso/NGC/2100-2200/IC2177_300u350.md b/cs/dso/NGC/2100-2200/IC2177_300u350.md index 2cc635989..be7c8cffe 100644 --- a/cs/dso/NGC/2100-2200/IC2177_300u350.md +++ b/cs/dso/NGC/2100-2200/IC2177_300u350.md @@ -4,6 +4,6 @@ rating: created_by: editor.cs created_date: 2020-09-23 20:52:14.281965 updated_by: skybber -updated_date: 2021-01-25 18:28:21.723192 +updated_date: 2023-01-07 14:35:30.152351 --- 100x: IC 2177 je velkým dlouhým pásem mlhoviny, který se rozšiřuje severně do Jednorožce, blízko otevřené hvězdokupy NGC 2335 a jižně k hvězdě 8mag centrováná na Cederblad 90 (její nejzřejmější koncentrace). IC 2177 se může blýsknout pod tmavou průzračnou oblohou v triedru 10 × 50. V dalekohledu vyžaduje co nejmenší zvětšení a UHC, O-III nebo nejlépe H-beta filtr. Centrální část IC 2177 má samostatné označení NGC 2327 a je pozorována 35' západně od Struve 1026 (5,7mag, 9,1mag, 17,8 "). Je slabou, matnou, ale poměrně dost koncentrovanou reflexní mlhovinou, která nejlépe vynikne v H-beta filtru, obklopující hvězdu 10mag. Trochu lépe je vidět ve větších dalekohledech. \ No newline at end of file diff --git a/cs/dso/NGC/2100-2200/NGC2175.md b/cs/dso/NGC/2100-2200/NGC2175.md index 0a373ea8c..ce3cb3fa7 100644 --- a/cs/dso/NGC/2100-2200/NGC2175.md +++ b/cs/dso/NGC/2100-2200/NGC2175.md @@ -1,6 +1,6 @@ --- name: Opičí hlava -rating: 1 +rating: 7 references: created_by: skybber created_date: 2022-09-27 20:28:49.336084 diff --git a/cs/dso/NGC/2100-2200/NGC2175_300u350.md b/cs/dso/NGC/2100-2200/NGC2175_300u350.md index a0af047f7..91aaf23b9 100644 --- a/cs/dso/NGC/2100-2200/NGC2175_300u350.md +++ b/cs/dso/NGC/2100-2200/NGC2175_300u350.md @@ -4,6 +4,6 @@ rating: 1 created_by: skybber created_date: 2022-09-27 20:28:49.339326 updated_by: skybber -updated_date: 2022-09-27 20:28:49.340680 +updated_date: 2022-12-07 18:49:06.312137 --- velmi jasná s filtrem, velmi velká, obklopuje hvězdu 8. velikosti, obloha na západní straně velmi tmavá. Západně od hvězdy je mlhovina skvrnitá a pruhovaná s jasnou oblastí u severního okraje. diff --git a/cs/dso/NGC/2100-2200/NGC2175_400u500.md b/cs/dso/NGC/2100-2200/NGC2175_400u500.md index 14326eb25..e2a080a85 100644 --- a/cs/dso/NGC/2100-2200/NGC2175_400u500.md +++ b/cs/dso/NGC/2100-2200/NGC2175_400u500.md @@ -4,7 +4,7 @@ rating: 1 created_by: skybber created_date: 2022-09-27 20:28:49.339664 updated_by: skybber -updated_date: 2022-09-27 20:28:49.340776 +updated_date: 2022-12-07 18:49:06.312220 --- při zvětšení 64x a filtru OIII se jedná o krásnou, detailní mlhovinu obklopující hvězdu 8. mag (SAO 78049), která se rozprostírá nejméně v průměru 20'. Filtr OIII poskytuje dramatické zvýšení kontrastu. Při odvráceném pohledu a pečlivém pozorování sahají vnější hranice až do vzdálenosti ~25'. Struktura zahrnuje vnitřní pruhované tmavé pruhy viditelné západně od hvězdy. Okraj je o něco jasnější nebo má vyšší kontrast na západním okraji, ale na následující straně hvězdy je vidět o něco více mlhoviny. diff --git a/cs/dso/NGC/2300-2400/IC2375.md b/cs/dso/NGC/2300-2400/IC2375.md new file mode 100644 index 000000000..6e039f009 --- /dev/null +++ b/cs/dso/NGC/2300-2400/IC2375.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-26 10:40:11.886736 +updated_by: +updated_date: 2022-12-22 08:32:19.508386 +--- diff --git a/cs/dso/NGC/2300-2400/IC2375_400u500.md b/cs/dso/NGC/2300-2400/IC2375_400u500.md new file mode 100644 index 000000000..44fb3fe2f --- /dev/null +++ b/cs/dso/NGC/2300-2400/IC2375_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:40:11.890021 +updated_by: skybber +updated_date: 2022-12-26 10:40:11.891111 +--- +první a nejjasnější z těsné trojice s IC 2377 1,6' V a IC 2379 2,1' VSV. Slabá, středně velká, protáhlá 3:1 V-Z, 1,5'x0,5', rovnoměrně jasná na povrchu. Skupina leží poblíž dvou hvězd 11. mag orientovaných JZ-SV. diff --git a/cs/dso/NGC/2300-2400/IC2375_600u800.md b/cs/dso/NGC/2300-2400/IC2375_600u800.md new file mode 100644 index 000000000..1bfa27654 --- /dev/null +++ b/cs/dso/NGC/2300-2400/IC2375_600u800.md @@ -0,0 +1,11 @@ +--- +aperture: 600/800 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:40:11.890357 +updated_by: skybber +updated_date: 2022-12-26 10:40:11.891209 +--- +první z nápadné trojice IC galaxií. Při 322x; jeví se jako poměrně slabá až středně jasná, poměrně malá, velmi protáhlá 7:2 V-Z, 0,8'x0,25'. IC 2377 leží 1,6' V a IC 2379 2,1' VJV. + +Kromě toho jsem zachytil MCG -02-22-011 14' JJZ (stejný červený posuv jako triplet; kvarteto tvořící LDCE 574). MCG -02-22-011 byla srovnatelná s IC a jevila se poměrně slabá, malá, protáhlá 5:3 S-J, ~25"x15", malé jasné jádro. Hvězda 12,3 mag se nachází mimo jihovýchodní stranu [30" od středu]. \ No newline at end of file diff --git a/cs/dso/NGC/2300-2400/NGC2345.md b/cs/dso/NGC/2300-2400/NGC2345.md index e1754ec73..489692a7e 100644 --- a/cs/dso/NGC/2300-2400/NGC2345.md +++ b/cs/dso/NGC/2300-2400/NGC2345.md @@ -5,6 +5,6 @@ references: created_by: editor.cs created_date: 2020-09-23 20:52:01.604110 updated_by: skybber -updated_date: 2021-01-09 10:11:32.999098 +updated_date: 2022-12-04 09:33:35.491422 --- -![<]($IMG_DIR/dso/NGC2345.jpg) +![<]($IMG_DIR/dso/NGC2345.jpg) diff --git a/cs/dso/NGC/2300-2400/NGC2345_200u250.md b/cs/dso/NGC/2300-2400/NGC2345_200u250.md index 1f685a248..925e58076 100644 --- a/cs/dso/NGC/2300-2400/NGC2345_200u250.md +++ b/cs/dso/NGC/2300-2400/NGC2345_200u250.md @@ -4,6 +4,6 @@ rating: 1 created_by: skybber created_date: 2021-01-09 10:11:32.693168 updated_by: skybber -updated_date: 2021-01-09 10:11:32.999319 +updated_date: 2022-12-04 09:33:35.491275 --- Otevřená hvězdokupa se v dalekohledu táhne jižně od hvězdy 8,5mag. Jedná se o skupinu 30 hvězd jasnosti 10-14mag. Jasnější členové tvoří seskupení "V", označené v SSV bodě dvojhvězdou. \ No newline at end of file diff --git a/cs/dso/NGC/2300-2400/NGC2345_300u350.md b/cs/dso/NGC/2300-2400/NGC2345_300u350.md index 4981c760d..9c711edb5 100644 --- a/cs/dso/NGC/2300-2400/NGC2345_300u350.md +++ b/cs/dso/NGC/2300-2400/NGC2345_300u350.md @@ -4,6 +4,6 @@ rating: 1 created_by: skybber created_date: 2021-01-09 10:11:32.757775 updated_by: skybber -updated_date: 2021-01-09 10:11:32.999438 +updated_date: 2022-12-04 09:33:35.491348 --- -V dalekohledu se jedná o poměrně jasnou, velkou, uvolněnou, nepravidelnou kopu asi 50 hvězd, jasnosti většinou 11mag a slabších. Nejjasnější hvězdy kupy, jihozápadně od hlavní koncentrace, připomínají osten šípu směřující do prázdném oblasti. Hvězda na jeho špici je nádhernou dvojhvězdou, tvořenou modrozelenou (10mag) a oranžovou složkou (11mag). Tři hvězdy podél východní strany hlavy šípu mají všechny společníků, střední z nich je navíc trojhvězdí. \ No newline at end of file +V dalekohledu se jedná o poměrně jasnou, velkou, uvolněnou, nepravidelnou kupu asi 50 hvězd, jasnosti většinou 11mag a slabších. Nejjasnější hvězdy kupy, jihozápadně od hlavní koncentrace, připomínají osten šípu směřující do prázdném oblasti. Hvězda na jeho špici je nádhernou dvojhvězdou, tvořenou modrozelenou (10mag) a oranžovou složkou (11mag). Tři hvězdy podél východní strany hlavy šípu mají všechny společníků, střední z nich je navíc trojhvězdí. \ No newline at end of file diff --git a/cs/dso/NGC/2300-2400/NGC2392.md b/cs/dso/NGC/2300-2400/NGC2392.md index ede669319..5daf8b70f 100644 --- a/cs/dso/NGC/2300-2400/NGC2392.md +++ b/cs/dso/NGC/2300-2400/NGC2392.md @@ -5,7 +5,7 @@ references: created_by: editor.cs created_date: 2020-09-23 20:52:01.541333 updated_by: skybber -updated_date: 2021-01-09 14:22:01.634845 +updated_date: 2022-12-17 08:54:36.469424 --- -![<]($IMG_DIR/dso/NGC2392.jpg) -Planetární mlhovina nedaleko δ Gem, objevená v roce 1787 W. Herschelem. Název "Eskymák" nebo "Klaun" získala podle barevných fotografií, na kterých při troše fantazie připomíná lidskou tvář v kožešině. Vzdálená je přibližně 6 500 ly. Mlhovina je dostatečně jasná i při pozorování z osvětlených míst, její jas je totiž koncentrovaný v malé ploše. Na zkoumání tedy potřebujeme použít velké zvětšení. Má malý ale jasný kruhový modravý disk, ve kterém se nachází i centrální hvězda (10,5mag). +![<]($IMG_DIR/dso/NGC2392.jpg) +Planetární mlhovina nedaleko δ Gem, objevená v roce 1787 W. Herschelem. Název "Eskymák" nebo "Klaun" získala podle barevných fotografií, na kterých při troše fantazie připomíná lidskou tvář v kožešině. Vzdálená je přibližně 6 500 ly. Mlhovina je dostatečně jasná i při pozorování z osvětlených míst, její jas je totiž koncentrovaný v malé ploše. Na zkoumání tedy potřebujeme použít velké zvětšení. Má malý ale jasný kruhový modravý disk, ve kterém se nachází i centrální hvězda (10,5mag). diff --git a/cs/dso/NGC/2300-2400/NGC2392_200u250.md b/cs/dso/NGC/2300-2400/NGC2392_200u250.md index e4e3553f8..43cc463b6 100644 --- a/cs/dso/NGC/2300-2400/NGC2392_200u250.md +++ b/cs/dso/NGC/2300-2400/NGC2392_200u250.md @@ -3,7 +3,7 @@ aperture: 200/250 rating: created_by: editor.cs created_date: 2020-09-23 20:52:09.668217 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:09.668246 +updated_by: skybber +updated_date: 2022-12-17 08:54:36.469243 --- -je modravý odstín zřejmý, navíc působí i "blikající efekt". 250x zvětšení odhalí nezřetelný tmavý prstenec v poloviční vzdálenosti od centra směrem k okraji. \ No newline at end of file +její modravý odstín je zřetený, navíc působí i "blikající efekt". 250x zvětšení odhalí nezřetelný tmavý prstenec v poloviční vzdálenosti od centra směrem k okraji. \ No newline at end of file diff --git a/cs/dso/NGC/2300-2400/NGC2392_400u500.md b/cs/dso/NGC/2300-2400/NGC2392_400u500.md index 8b3e3ac53..b2c41113c 100644 --- a/cs/dso/NGC/2300-2400/NGC2392_400u500.md +++ b/cs/dso/NGC/2300-2400/NGC2392_400u500.md @@ -4,7 +4,7 @@ rating: created_by: editor.cs created_date: 2020-09-23 20:52:09.731593 updated_by: skybber -updated_date: 2021-01-09 12:57:21.590526 +updated_date: 2022-12-17 08:54:36.469356 --- -600x, [OIII] filtr, 6m5 +600x, [OIII] filtr, 6m5 Při vysokém zvětšení 600x a [OIII] se mlhovina rozpadá na ostře ohraničený, asymetrický prstenec obklopující jasnou centrální hvězdu s okolní kulatou vnější oblastí. Prstenec je nejjasnější na západní straně, následovaný východní stranou, slabší na severu a na jihu, Obzvláště je široký na severu. Tvar prstence je mírně eliptický a zužuje se směrem k severu, zatímco na jihu je téměř rovný. Jasné struktury v NII a H-alfa ve vnějším prstenci nejsou vizuálně vnímatelné, ale lze vidět malé rozdíly v jasu. Nejnápadnější je široká zakřivená oblast 1:3 východ-západ na jižním okraji. Na severní hranici je také jasnější pás mírně odsazený k severovýchodu. Na západním okraji je velmi slabě vidět zjasnění. \ No newline at end of file diff --git a/cs/dso/NGC/2400-2500/NGC2479.md b/cs/dso/NGC/2400-2500/NGC2479.md new file mode 100644 index 000000000..9747d6df8 --- /dev/null +++ b/cs/dso/NGC/2400-2500/NGC2479.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-26 10:32:41.008534 +updated_by: +updated_date: 2022-12-22 08:32:19.508386 +--- diff --git a/cs/dso/NGC/2400-2500/NGC2479_300u350.md b/cs/dso/NGC/2400-2500/NGC2479_300u350.md new file mode 100644 index 000000000..5d280cfdd --- /dev/null +++ b/cs/dso/NGC/2400-2500/NGC2479_300u350.md @@ -0,0 +1,9 @@ +--- +aperture: 300/350 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:32:41.010869 +updated_by: skybber +updated_date: 2022-12-26 10:32:41.012160 +--- +asi 50 slabých hvězd rozprostřených v průměru 10' nad mlhou. Několik hvězd poblíž středu je uspořádáno do půlkruhu otevřeného na východní straně. Na JV se táhne řetěz hvězd. \ No newline at end of file diff --git a/cs/dso/NGC/2400-2500/NGC2479_400u500.md b/cs/dso/NGC/2400-2500/NGC2479_400u500.md new file mode 100644 index 000000000..c50171997 --- /dev/null +++ b/cs/dso/NGC/2400-2500/NGC2479_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:32:41.011202 +updated_by: skybber +updated_date: 2022-12-26 10:32:41.012235 +--- +175x více než 80 hvězd mag 12-14 rozlišeno v 9' oblasti s hvězdokupou protáhlou ZJZ-VSV. Půlkruhová smyčka hvězd je blízko středu a je otevřená na východní straně. Hvězdokupa se nachází ~10' SV od poměrně dobře sladěného, jasného širokého páru (h4015 = 9,1/9,5 při 20"). \ No newline at end of file diff --git a/cs/dso/NGC/2400-2500/NGC2489.md b/cs/dso/NGC/2400-2500/NGC2489.md new file mode 100644 index 000000000..3572b3a48 --- /dev/null +++ b/cs/dso/NGC/2400-2500/NGC2489.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-26 10:30:51.682381 +updated_by: +updated_date: 2022-12-22 08:32:19.508386 +--- diff --git a/cs/dso/NGC/2400-2500/NGC2489_300u350.md b/cs/dso/NGC/2400-2500/NGC2489_300u350.md new file mode 100644 index 000000000..08f94ca33 --- /dev/null +++ b/cs/dso/NGC/2400-2500/NGC2489_300u350.md @@ -0,0 +1,9 @@ +--- +aperture: 300/350 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:30:51.684512 +updated_by: skybber +updated_date: 2022-12-26 10:30:51.685731 +--- +asi 50 hvězd o průměru 8'. Bohatá na hvězdy 11-14 mag. Bohatší skupina hvězd je uprostřed obklopena větším neúplným prstencem hvězd. Nachází se 13' severně od PX Puppis (6,3-6,7). \ No newline at end of file diff --git a/cs/dso/NGC/2500-2600/NGC2525.md b/cs/dso/NGC/2500-2600/NGC2525.md new file mode 100644 index 000000000..feb1261b2 --- /dev/null +++ b/cs/dso/NGC/2500-2600/NGC2525.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-26 10:36:55.434375 +updated_by: +updated_date: 2022-12-22 08:36:08.269263 +--- diff --git a/cs/dso/NGC/2500-2600/NGC2525_300u350.md b/cs/dso/NGC/2500-2600/NGC2525_300u350.md new file mode 100644 index 000000000..becc3ce1f --- /dev/null +++ b/cs/dso/NGC/2500-2600/NGC2525_300u350.md @@ -0,0 +1,9 @@ +--- +aperture: 300/350 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:36:55.445044 +updated_by: skybber +updated_date: 2022-12-26 10:37:13.498355 +--- +poměrně slabá, velká, mírně protáhlá V-Z, rozptýlený, slabě koncentrovaná. Nachází se 3,8' SZ od SAO 153813 mag 8,9 a 6,2' J od SAO 153816 mag 8,7 na hranici Jednorožce. diff --git a/cs/dso/NGC/2500-2600/NGC2525_600u800.md b/cs/dso/NGC/2500-2600/NGC2525_600u800.md new file mode 100644 index 000000000..56707b197 --- /dev/null +++ b/cs/dso/NGC/2500-2600/NGC2525_600u800.md @@ -0,0 +1,9 @@ +--- +aperture: 600/800 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:36:55.447068 +updated_by: skybber +updated_date: 2022-12-26 10:37:13.498478 +--- + 200x a 375x; poměrně jasná, poměrně velká, oválná 4:3 ~V-Z, široká koncentrace, při 200x bez zřetelného jádra, ale halo se zdálo být skvrnité nebo nerovnoměrné (jasnější a tmavší oblasti), silně naznačující spirální strukturu. Při 375x byl viditelný krátká málo kontrastní centrální příčka (protáhlá zhruba 3:1 V-Z) s mírně jasnějším jádrem. diff --git a/cs/dso/NGC/2500-2600/NGC2568.md b/cs/dso/NGC/2500-2600/NGC2568.md new file mode 100644 index 000000000..ad6caa1a1 --- /dev/null +++ b/cs/dso/NGC/2500-2600/NGC2568.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-26 10:34:39.761287 +updated_by: +updated_date: 2022-12-22 08:32:19.508386 +--- diff --git a/cs/dso/NGC/2500-2600/NGC2568_300u350.md b/cs/dso/NGC/2500-2600/NGC2568_300u350.md new file mode 100644 index 000000000..b2f59bc81 --- /dev/null +++ b/cs/dso/NGC/2500-2600/NGC2568_300u350.md @@ -0,0 +1,9 @@ +--- +aperture: 300/350 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:34:39.763656 +updated_by: skybber +updated_date: 2022-12-26 10:34:39.764953 +--- +malá, slabá skupina asi 6 hvězd nad nerozlišenou difuzí, nevýrazná. \ No newline at end of file diff --git a/cs/dso/NGC/2500-2600/NGC2571.md b/cs/dso/NGC/2500-2600/NGC2571.md new file mode 100644 index 000000000..224ffbae5 --- /dev/null +++ b/cs/dso/NGC/2500-2600/NGC2571.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-26 10:29:28.695629 +updated_by: +updated_date: 2022-12-22 08:32:19.508386 +--- diff --git a/cs/dso/NGC/2500-2600/NGC2571_300u350.md b/cs/dso/NGC/2500-2600/NGC2571_300u350.md new file mode 100644 index 000000000..99bf60e84 --- /dev/null +++ b/cs/dso/NGC/2500-2600/NGC2571_300u350.md @@ -0,0 +1,9 @@ +--- +aperture: 300/350 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:29:28.697710 +updated_by: skybber +updated_date: 2022-12-26 10:29:28.699189 +--- +18 hvězd mag 8,8-12 v průměru 10'. Zahrnuje širokou jasnou dvojici (SAO 175580 mag 8,8 a SAO 175577 mag 8,9) ve vzdálenosti 1' orientovanou SZ-JV poblíž středu. Tato hvězdokupa je větší a obsahuje jasnější hvězdy než NGC 2587 o jeden stupeň východněji. 47' JV leží také NGC 2580 a 54' JV NGC 2567 J. \ No newline at end of file diff --git a/cs/dso/NGC/2500-2600/NGC2571_400u500.md b/cs/dso/NGC/2500-2600/NGC2571_400u500.md new file mode 100644 index 000000000..b9fc24d0f --- /dev/null +++ b/cs/dso/NGC/2500-2600/NGC2571_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:29:28.698014 +updated_by: skybber +updated_date: 2022-12-26 10:29:28.699264 +--- +velmi zajímavá hvězdokupa s ~30 hvězdami v jádru hvězdokupy, včetně dvou hvězd 9. mag, HD 70058 a 70078, orientovaných SZ-JV a velkého počtu hvězd 10.-11. magnitudy. Hvězdy "jádra" jsou dosti izolovány širokým, většinou prázdným prstencem, ve kterém jsou jen mnohem slabší hvězdy. V poloměru 4' od středu se nachází výrazný řetězec hvězd na SZ (orientovaný JZ-SV) a rozsáhlá skupina hvězd na jihu, které mohou být také součástí hvězdokupy. Započtením velké skupiny až do průměru 13' se celkový počet hvězd zvýší na 100-120 (i když velká část z nich jsou hvězdy nesouvisející), ale zdá se, že je příliš rozvolněná na to, aby byla při této velikosti zřetelná. Tato oblast Mléčné dráhy je bohatá na jasné i slabé hvězdy: hvězda 7. mag (HD 69817) je 17' ZSZ a hvězdy 6-7. mag jsou 20' JZ a 20' SV. \ No newline at end of file diff --git a/cs/dso/NGC/300-400/IC349.md b/cs/dso/NGC/300-400/IC349.md new file mode 100644 index 000000000..3836d2f2a --- /dev/null +++ b/cs/dso/NGC/300-400/IC349.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-03 18:50:25.282975 +updated_by: +updated_date: 2022-12-03 18:39:04.039392 +--- diff --git a/cs/dso/NGC/300-400/IC349_900u1200.md b/cs/dso/NGC/300-400/IC349_900u1200.md new file mode 100644 index 000000000..72b1fac20 --- /dev/null +++ b/cs/dso/NGC/300-400/IC349_900u1200.md @@ -0,0 +1,9 @@ +--- +aperture: 900/1200 +rating: 1 +created_by: skybber +created_date: 2022-12-03 18:50:25.288030 +updated_by: skybber +updated_date: 2022-12-03 18:50:25.288420 +--- + IC 349 je reflexní uzel jen 36" JJV od Merope. Použili jsme 813x a pečlivě jsme Merope umístili sotva za severní okraj pole. Orientaci bylo snadné posoudit podle dvou hvězd 15mag 1,8' S a 1,8' JJZ od Merope a protáhlá záře spadala mezi difrakční kříže. Navzdory oslnění od Merope, které pozorování značně ztěžovalo, mě překvapilo, že tato malá reflexní mlhovina byla poměrně jasná a protáhlá (zhruba směřovala jižně od Merope) s rovnějším západním okrajem o velikosti snad 20"x10". diff --git a/cs/dso/NGC/3000-3100/NGC3047.md b/cs/dso/NGC/3000-3100/NGC3047.md new file mode 100644 index 000000000..4b62c8b79 --- /dev/null +++ b/cs/dso/NGC/3000-3100/NGC3047.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-26 10:26:30.128928 +updated_by: +updated_date: 2022-12-22 08:32:19.508386 +--- diff --git a/cs/dso/NGC/3000-3100/NGC3047_400u500.md b/cs/dso/NGC/3000-3100/NGC3047_400u500.md new file mode 100644 index 000000000..ebf44e9c6 --- /dev/null +++ b/cs/dso/NGC/3000-3100/NGC3047_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:26:30.131276 +updated_by: skybber +updated_date: 2022-12-26 10:26:30.132239 +--- +velmi slabá, velmi malá, kulaté, slabé hvězdné jádro o průměru 15". Nachází se 1,3' JJV od SAO 137215 mag 8,6. Tvoří dvojitý systém s velmi slabým hvězdným společníkem (NGC 3047A) jen 40" ZSZ od středu. \ No newline at end of file diff --git a/cs/dso/NGC/3100-3200/NGC3156.md b/cs/dso/NGC/3100-3200/NGC3156.md new file mode 100644 index 000000000..5298a252c --- /dev/null +++ b/cs/dso/NGC/3100-3200/NGC3156.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-26 10:11:44.562456 +updated_by: +updated_date: 2022-12-22 08:32:19.508386 +--- diff --git a/cs/dso/NGC/3100-3200/NGC3156_300u350.md b/cs/dso/NGC/3100-3200/NGC3156_300u350.md new file mode 100644 index 000000000..115a9154a --- /dev/null +++ b/cs/dso/NGC/3100-3200/NGC3156_300u350.md @@ -0,0 +1,9 @@ +--- +aperture: 300/350 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:11:44.564489 +updated_by: skybber +updated_date: 2022-12-26 10:11:44.565986 +--- +slabá, malá, protáhlá. \ No newline at end of file diff --git a/cs/dso/NGC/3100-3200/NGC3156_400u500.md b/cs/dso/NGC/3100-3200/NGC3156_400u500.md new file mode 100644 index 000000000..1789d1ce0 --- /dev/null +++ b/cs/dso/NGC/3100-3200/NGC3156_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:11:44.564812 +updated_by: skybber +updated_date: 2022-12-26 10:11:44.566088 +--- +středně jasná, malá, malé jasné jádro. Následuje trojúhelník jasných hvězd: SAO 118165 mag 9,0 2,4' JV, SAO 118168 mag 8,3 5' VSV a SAO 118169 mag 7,6 9' JV. \ No newline at end of file diff --git a/cs/dso/NGC/3100-3200/NGC3166_400u500.md b/cs/dso/NGC/3100-3200/NGC3166_400u500.md index 156b831e8..788912aaf 100644 --- a/cs/dso/NGC/3100-3200/NGC3166_400u500.md +++ b/cs/dso/NGC/3100-3200/NGC3166_400u500.md @@ -4,6 +4,6 @@ rating: 1 created_by: skybber created_date: 2022-02-14 20:46:44.155419 updated_by: skybber -updated_date: 2022-02-14 20:46:44.368277 +updated_date: 2023-03-16 09:45:18.585053 --- -jasná, téměř kulatá, rovnoměrně koncentrovaná do jasnějšího jádra a hvězdného jádra (velká ramena s nízkou povrchovou jasností nejsou vidět). Jádro se zdá být jasnější než NGC 3169 7,8' východně, ale duo je dosti podobné. Druhá ze tří hvězd s NGC 3165 4,6' JZ. Dvě hvězdy 12,5 mag leží 2,6' SZ a 2,8' JZ od středu. \ No newline at end of file +jasná, téměř kulatá, rovnoměrně koncentrovaná do jasnějšího jádra a hvězdného jadérka (velká ramena s nízkou povrchovou jasností nejsou vidět). Jádro se zdá být jasnější než NGC 3169 7,8' východně, ale duo je dosti podobné. Druhá ze tří hvězd s NGC 3165 4,6' JZ. Dvě hvězdy 12,5 mag leží 2,6' SZ a 2,8' JZ od středu. \ No newline at end of file diff --git a/cs/dso/NGC/3200-3300/NGC3247.md b/cs/dso/NGC/3200-3300/NGC3247.md new file mode 100644 index 000000000..d826914ba --- /dev/null +++ b/cs/dso/NGC/3200-3300/NGC3247.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-04 10:32:51.378312 +updated_by: +updated_date: 2022-12-04 09:16:10.642221 +--- diff --git a/cs/dso/NGC/3200-3300/NGC3247_300u350.md b/cs/dso/NGC/3200-3300/NGC3247_300u350.md new file mode 100644 index 000000000..16bc1346b --- /dev/null +++ b/cs/dso/NGC/3200-3300/NGC3247_300u350.md @@ -0,0 +1,9 @@ +--- +aperture: 300/350 +rating: 1 +created_by: skybber +created_date: 2022-12-04 10:32:51.380396 +updated_by: skybber +updated_date: 2022-12-04 10:32:51.381896 +--- +NGC 3247 se skládá z kompaktní hvězdokupy (často označované jako Westerlund 2), jedné z nejhmotnějších známých mladých hvězdokup v Mléčné dráze, a velké nepravidelné oblasti H II (RCW 49) s hvězdotvornými pilíři podobnými Orlí mlhovině. Při zvětšení 230x se hvězdokupa táhla ~1,5', ale nejbohatší částí byl hustý protáhlý chuchvalec dlouhý pouhých 45" s půltuctem těsně na sebe nabalených hvězd mag 13,5-14 rozlišených v řetězci ZSZ-VJV. Na JZ straně se nachází WR 20a mag 13,5, jeden z nejhmotnějších binárních systémů (obě hvězdy jsou nadsvítivé typu O3). Hvězdokupa se nachází 12' SZ od HD 90289 mag 5,8. \ No newline at end of file diff --git a/cs/dso/NGC/3300-3400/NGC3372.md b/cs/dso/NGC/3300-3400/NGC3372.md index 99ac47809..de6d5c5b1 100644 --- a/cs/dso/NGC/3300-3400/NGC3372.md +++ b/cs/dso/NGC/3300-3400/NGC3372.md @@ -5,12 +5,12 @@ references: created_by: editor.cs created_date: 2020-09-23 20:52:02.792846 updated_by: skybber -updated_date: 2020-09-29 11:45:27.419787 +updated_date: 2023-01-07 20:44:19.547796 --- -![<]($IMG_DIR/dso/NGC3372.jpg) - -Pokud se podíváme do zorného pole dalekohledu na hvězdu η Carinae, určitě snadno zjistíme, že je obklopena rozsáhlou a jasnou emisní mlhovinou NGC 3372, nazvanou rovněž η Carinae, nádherně viditelnou oproti Mléčné silnici i pouhým okem jako světlá velká skvrna prodloužena v poměru 2: 1 . Je naší nejjasnější částí ionizovaného vodíku a na obloze v prostoru Mléčné dráhy zabírá plochu asi čtyř stupňů. Z praktického hlediska to znamená, že už v triedru ji můžete obdivovat tak jako Velkou mlhovinu v Orionu v dalekohledu! Je popredkávaná jemnými mlhovinový závoji. Prochází ní i pás tmavého prachu, který má tvar písmene "V" a rozděluje ji tak brzy na polovinu. Nejvýraznější tmavý oblak prachu, skutečně nepřehlédnutelná temná mlhovina se nazývá **Klíčová dírka - NGC 3324 (Keyhole nebula)**. Kolem oranžové hvězdy η Carinae se zase rozkládá nápadná jasná skvrna široká asi 15 minut nazývaná Trpaslík. Celá mlhovina má průměr asi 400 světelných let. - -Triedr 10 × 50 v mlhovině rozliší desítku hvězd s náznakem dalších a bočním pohledem se odkryjí i slabší vnější části tohoto pozoruhodného objektu. - -![<]($IMG_DIR/dso/NGC3372-center.jpg) +![<]($IMG_DIR/dso/NGC3372.jpg) + +Pokud se podíváme do zorného pole dalekohledu na hvězdu η Carinae, určitě snadno zjistíme, že je obklopena rozsáhlou a jasnou emisní mlhovinou NGC 3372, nazvanou rovněž η Carinae, nádherně viditelnou oproti Mléčné silnici i pouhým okem jako světlá velká skvrna prodloužena v poměru 2: 1 . Je naší nejjasnější částí ionizovaného vodíku a na obloze v prostoru Mléčné dráhy zabírá plochu asi čtyř stupňů. Z praktického hlediska to znamená, že už v triedru ji můžete obdivovat tak jako Velkou mlhovinu v Orionu v dalekohledu! Je prodkaná jemnými mlhovinový závoji. Prochází skrz ní i pás tmavého prachu, který má tvar písmene "V" a rozděluje ji tak na polovinu. Nejvýraznější tmavý oblak prachu, skutečně nepřehlédnutelná temná mlhovina se nazývá **Klíčová dírka - NGC 3324 (Keyhole nebula)**. Kolem oranžové hvězdy η Carinae se zase rozkládá nápadná jasná skvrna široká asi 15 minut nazývaná Trpaslík. Celá mlhovina má průměr asi 400 světelných let. + +Triedr 10 × 50 v mlhovině rozliší desítku hvězd s náznakem dalších a bočním pohledem se odkryjí i slabší vnější části tohoto pozoruhodného objektu. + +![<]($IMG_DIR/dso/NGC3372-center.jpg) diff --git a/cs/dso/NGC/3300-3400/NGC3372_300u350.md b/cs/dso/NGC/3300-3400/NGC3372_300u350.md index 83d835f8a..ebf46e8e7 100644 --- a/cs/dso/NGC/3300-3400/NGC3372_300u350.md +++ b/cs/dso/NGC/3300-3400/NGC3372_300u350.md @@ -4,6 +4,6 @@ rating: 1 created_by: skybber created_date: 2020-09-29 11:45:27.413353 updated_by: skybber -updated_date: 2020-09-29 11:45:27.420008 +updated_date: 2023-01-07 20:44:19.547514 --- V dalekohledu se celá mlhovina nevejde do zorného pole. Je však tolerantní na větší zvětšení (i mlhovinový filtry), takže můžete zkoumat znamenité detaily. Různé dobře definované tmavé linie uvnitř mlhoviny jsou fascinující. Trpaslík je pěkný objekt při velmi dobrém seeingu. \ No newline at end of file diff --git a/cs/dso/NGC/400-500/IC412.md b/cs/dso/NGC/400-500/IC412.md new file mode 100644 index 000000000..28a518a38 --- /dev/null +++ b/cs/dso/NGC/400-500/IC412.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-07 18:58:53.094215 +updated_by: +updated_date: 2022-12-05 00:11:59.873325 +--- diff --git a/cs/dso/NGC/400-500/IC412_400u500.md b/cs/dso/NGC/400-500/IC412_400u500.md new file mode 100644 index 000000000..2438e5863 --- /dev/null +++ b/cs/dso/NGC/400-500/IC412_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-07 18:58:53.096794 +updated_by: skybber +updated_date: 2022-12-07 18:58:53.099162 +--- + toto je SZ člen neobvyklé těsné dvojice interagujících galaxií s IC 413 - vzdálenost pouhých 35" (v PA 115°) a oba členové jako by vycházeli z hvězdy 12. mag (30" od středu ke hvězdě)! Obě galaxie jsou slabé, velmi malé, mírně protáhlé, ~25 "x15", s malými jasnějšími jádry. IC 412 je protáhlá ve směru JJZ-SSV a 30" JZ od hvězdy 12. mag - se SV koncem těsně západně od hvězdy. Nachází se 6' JJZ od hvězdy SAO 112679 mag 7,6 a 14' ZJZ od dvojhvězdy 23 Orionis mag 5/7 (32"). Třetí galaxie, IC 414 , je v poli 8,5' J a tvoří chudou kupu galaxií WBL 114. diff --git a/cs/dso/NGC/400-500/IC412_600u800.md b/cs/dso/NGC/400-500/IC412_600u800.md new file mode 100644 index 000000000..9463b2e84 --- /dev/null +++ b/cs/dso/NGC/400-500/IC412_600u800.md @@ -0,0 +1,11 @@ +--- +aperture: 600/800 +rating: 1 +created_by: skybber +created_date: 2022-12-07 18:58:53.098282 +updated_by: skybber +updated_date: 2022-12-07 18:58:53.099263 +--- + oba členové této interagující dvojice (VV 225) jsou poměrně slabí, malí, zhruba 20-25" velcí, a každý z nich obsahuje malá jasná jádra. IC 412, SZ složka, je větší a protáhlejší, zhruba 5:3 JV-SZ, 25 "x15". IC 413 se nachází těsně u VJV strany, 35" mezi středy. Hvězda s mag 12,3 je 30" VSV od nás (na severním okraji IC 413 ). Protažené spirální rameno nebo slapový ohon na severu nebyl vidět. Dvojice se nachází 14' ZJZ od jasné dvojhvězdy 23 Ori = STF 696 (5,0/7,2 na 32"). IC 414 leží 8,5' J. + +Člen skupiny (WBL 114 = LGG 130) ve vzdálenosti ~180 milionů s.l. s UGC 3294 , 34' ZSZ. Tato spirála se jevila jako středně jasná a velká, obsahuje velmi difuzní halo s nízkou plošnou jasností snad 1,3'x0,6' SZ-JV s malým jasnějším jádrem, které se zvětšuje až do hvězdného jádra. Vnější halo mění vzhled při bočním pohledu (bez ostrého okraje) podle toho, jakou část zachytím. Nachází se 4' Z od hvězdy 6,5 mag HD 34959 a pohled na ni ovlivňuje oslnění - nejlépe s hvězdou umístěnou mimo zorné pole. diff --git a/cs/dso/NGC/400-500/IC447.md b/cs/dso/NGC/400-500/IC447.md new file mode 100644 index 000000000..8ec079575 --- /dev/null +++ b/cs/dso/NGC/400-500/IC447.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2023-01-07 14:18:52.247727 +updated_by: +updated_date: 2023-01-07 13:54:36.751951 +--- diff --git a/cs/dso/NGC/400-500/IC447_400u500.md b/cs/dso/NGC/400-500/IC447_400u500.md new file mode 100644 index 000000000..ac2a9a53b --- /dev/null +++ b/cs/dso/NGC/400-500/IC447_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2023-01-07 14:18:52.250250 +updated_by: skybber +updated_date: 2023-01-07 14:19:40.114885 +--- +při zvětšení 175x bez filtru se jedná o obrovskou, zajímavou reflexní mlhovinu, ~25'x18', protáhlou ve směru SZ-JV s nepravidelným obrysem a jemnými změnami jasnosti. Překrývá ji řada hvězd 8-10 mag, včetně hvězdy 8. mag HD 46005 (osvětlující hvězda), která je součástí 10' S-J řetězce čtyř jasnějších hvězd na východní straně. Mezi blízké reflexní mlhoviny patří NGC 2245 ~30' SV, IC 446 35' S a NGC 2247 40' SV (tato skupina tvoří asociaci Monoceros R1). \ No newline at end of file diff --git a/cs/dso/NGC/4300-4400/NGC4314_400u500.md b/cs/dso/NGC/4300-4400/NGC4314_400u500.md index 97a811962..79ba99c58 100644 --- a/cs/dso/NGC/4300-4400/NGC4314_400u500.md +++ b/cs/dso/NGC/4300-4400/NGC4314_400u500.md @@ -4,6 +4,6 @@ rating: 1 created_by: skybber created_date: 2022-02-11 22:37:54.687024 updated_by: skybber -updated_date: 2022-02-11 22:37:54.831366 +updated_date: 2023-05-09 12:06:26.910338 --- -poměrně jasná, poměrně velká, protáhlá ~3:1 SSZ-JJV, ~3'x1' [výrazný centrální pruh]. Halo na koncích slábne a poměrně prudce stoupá k oválnému jádru. V SZ cípu se nachází hvězda 13. mag a na jihovýchodní straně je zakotvena hvězda 14/15. mag. Slabé vnější halo této pruhované spirály nebylo vidět. \ No newline at end of file +poměrně jasná, poměrně velká, protáhlá ~3:1 SSZ-JJV, ~3'x1' [výrazná příčka]. Halo na koncích slábne a poměrně prudce stoupá k oválnému jádru. V SZ cípu se nachází hvězda 13. mag a na jihovýchodní straně je zakotvena hvězda 14/15. mag. Slabé vnější halo této pruhované spirály nebylo vidět. \ No newline at end of file diff --git a/cs/dso/NGC/500-600/IC575.md b/cs/dso/NGC/500-600/IC575.md new file mode 100644 index 000000000..6ee14cd74 --- /dev/null +++ b/cs/dso/NGC/500-600/IC575.md @@ -0,0 +1,9 @@ +--- +name: +rating: 1 +references: +created_by: skybber +created_date: 2022-12-26 10:10:11.022831 +updated_by: +updated_date: 2022-12-22 08:36:08.269263 +--- diff --git a/cs/dso/NGC/500-600/IC575_400u500.md b/cs/dso/NGC/500-600/IC575_400u500.md new file mode 100644 index 000000000..6fc7fa762 --- /dev/null +++ b/cs/dso/NGC/500-600/IC575_400u500.md @@ -0,0 +1,9 @@ +--- +aperture: 400/500 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:10:11.026753 +updated_by: skybber +updated_date: 2022-12-26 10:10:11.028171 +--- +246x jeví se jako poměrně slabá, poměrně malá, oválná 4:3 SZ-JV, ~28 "x21", jen velmi slabá široká koncentrace bez jádra nebo zón. Rozšíření pozorovaná ve 48" nebyla rozlišena. IC 574 leží 6' SSV. \ No newline at end of file diff --git a/cs/dso/NGC/500-600/IC575_900u1200.md b/cs/dso/NGC/500-600/IC575_900u1200.md new file mode 100644 index 000000000..9d87ac892 --- /dev/null +++ b/cs/dso/NGC/500-600/IC575_900u1200.md @@ -0,0 +1,11 @@ +--- +aperture: 900/1200 +rating: 1 +created_by: skybber +created_date: 2022-12-26 10:10:11.027567 +updated_by: skybber +updated_date: 2022-12-26 10:10:11.028345 +--- +tento neobvyklý systém má prachový pruh podél hlavní osy a disk podobný polárnímu prstenci. Galaxie se jeví jako poměrně jasný ovál, protáhlý 3:2 ve směru SZ-JV, 0,6'x0,4', s malým jasným jádrem. Prachový pás byl pouze v náznaku, ale na SZ a JV konci byly vidět úzké nástavce nebo hroty, přičemž JV nástavec byl jasnější. Hvězda 15,2 mag se nachází 1,3' SZ a dvě hvězdy 13. a 14,5 mag 2,3' JV a 1,7' JV. + +Jsou zde dva blízcí průvodci, ale zaznamenal jsem pouze 2MASX J09543313-0650143 1,2' N. IC 575 je uvedena jako kandidát na polární prstenec v publikaci Whitmore et al "New observations and a photographic atlas of polar-ring galaxies" (1990AJ....100.1489W). \ No newline at end of file diff --git a/cs/dso/Sh2/Sh2-276.md b/cs/dso/Sh2/Sh2-276.md index fa9463c32..aebb9a172 100644 --- a/cs/dso/Sh2/Sh2-276.md +++ b/cs/dso/Sh2/Sh2-276.md @@ -1,18 +1,18 @@ --- name: Barnardův oblouk -rating: 5 +rating: 7 references: created_by: editor.cs created_date: 2020-09-23 20:52:05.917442 updated_by: skybber -updated_date: 2020-09-28 11:45:12.053666 +updated_date: 2022-12-03 20:05:19.206363 --- -![<]($IMG_DIR/dso/Sh2-276.jpg) -Velkolepý objekt souhvězdí, mlhavý pás jako jedna z částí ohromného kruhu průměru 12 stupňů se středem v místech někde mezi pásem a mečem Orion. Je místem, kde se rodí nové hvězdy a ty pak toto místo opouštějí. I když patří mezi velmi těžké objekty, jeho nejjasnější části si na vynikající obloze pouhým okem všimlo už několik pozorovatelů, včetně W. S. Houstona. Pokud použijete filtr H-Beta, zakopnete o něj i v dalekohledu. Stačí pouze posouvat tubusem a o chvíli se sám dostane do zorného pole. Náznakově je vidět i jeho struktura, zúžení, rozšíření a nepatrná změna jasnosti v jednotlivých jeho částech. Nejjasnější je asi jeden stupeň severovýchodně od reflexní mlhoviny M78 a pak se táhne asi 4-5 stupňů na jih, kde se vytrácí. Druhá jasnější část se nachází v bodě asi tři stupně východně od alnitak. - -Myzer: Musím říct, že Barnardův oblouk s filtrem H-Beta nepovažuji za velmi těžký objekt, příkladem může být jedno pozorování po Vánocích 2006 v Modre ze Somet Monart: V zorném poli tří stupňů byl oblouk nejsnáze rozeznatelný severně od reflexní mlhoviny M78, kde se nachází jeho nejužší a pravděpodobně i nejkontrastnějším část. V této části byl oblouk poměrně nápadný a s docela dobře definovatelnými hranicemi. Druhá pozorovatelná část se nacházela přímo východně od hvězdy Dzétou Orionis, v místech kde oblouk vykazuje svou největší šířku. Tato část měla sice už trochu slabší plošnou jasnost a méně jednoznačné hranice, přesto však zůstávala ještě rozeznatelná. Spojení obou zmíněných částí se přitom dalo pozorovat jen velmi náznakově, přesto je to slušný výkon pokud zohledníme skutečnost, že Barnardův oblouk se z Modry při kulminaci ve výši zhruba 50 stupňů ocitá ve směru 30 km vzdálené Bratislavy! Zmínit je třeba i skutečnost, že popisované části byly pozorovatelné i s UHC filtrem, přesto bychom je ale pravděpodobně nerozozoznali bez jejich předchozího vidění pomocí H-Beta filtru. Části jižně od pásu jsme překvapivě neviděli ani na La Palme (pravděpodobně mají jiné emisní vlastnosti a není vhodný H-Beta filtr). - -Dominik: Jedno úspěšné pozorování u Pavouka na Cerové mi vyvrátilo řeči, že tento objekt je obtížné pozorování. Na tento objekt jsem se velmi těšil, protože jsem o něm vždy jen slyšel mluvit a četl jsem o něm reporty, které většinou hovořily o náročnosti pozorování tohoto objektu. Avšak náročnost se mi nepotvrdila, Pavouk mi nastavil oblouk do zorného pole s H-beta filtrem a já jsem se jen divil. Byl to jasný šedý pás přes zorné pole, žádná nenápadná změna kontrastu, ale normální jasný oblak. Oblouk jsem si mohl pohybováním dalekohledu podívat celý a je to pozoruhodný pohled! - - - +![<]($IMG_DIR/dso/Sh2-276.jpg) +Velkolepý objekt souhvězdí, mlhavý pás jako jedna z částí ohromného kruhu průměru 12 stupňů se středem v místech někde mezi pásem a mečem Orion. Je místem, kde se rodí nové hvězdy a ty pak toto místo opouštějí. I když patří mezi velmi těžké objekty, jeho nejjasnější části si na vynikající obloze pouhým okem všimlo už několik pozorovatelů, včetně W. S. Houstona. Pokud použijete filtr H-Beta, zakopnete o něj i v dalekohledu. Stačí pouze posouvat tubusem a o chvíli se sám dostane do zorného pole. Náznakově je vidět i jeho struktura, zúžení, rozšíření a nepatrná změna jasnosti v jednotlivých jeho částech. Nejjasnější je asi jeden stupeň severovýchodně od reflexní mlhoviny M78 a pak se táhne asi 4-5 stupňů na jih, kde se vytrácí. Druhá jasnější část se nachází v bodě asi tři stupně východně od alnitak. + +Myzer: Musím říct, že Barnardův oblouk s filtrem H-Beta nepovažuji za velmi těžký objekt, příkladem může být jedno pozorování po Vánocích 2006 v Modre ze Somet Monart: V zorném poli tří stupňů byl oblouk nejsnáze rozeznatelný severně od reflexní mlhoviny M78, kde se nachází jeho nejužší a pravděpodobně i nejkontrastnějším část. V této části byl oblouk poměrně nápadný a s docela dobře definovatelnými hranicemi. Druhá pozorovatelná část se nacházela přímo východně od hvězdy Dzétou Orionis, v místech kde oblouk vykazuje svou největší šířku. Tato část měla sice už trochu slabší plošnou jasnost a méně jednoznačné hranice, přesto však zůstávala ještě rozeznatelná. Spojení obou zmíněných částí se přitom dalo pozorovat jen velmi náznakově, přesto je to slušný výkon pokud zohledníme skutečnost, že Barnardův oblouk se z Modry při kulminaci ve výši zhruba 50 stupňů ocitá ve směru 30 km vzdálené Bratislavy! Zmínit je třeba i skutečnost, že popisované části byly pozorovatelné i s UHC filtrem, přesto bychom je ale pravděpodobně nerozozoznali bez jejich předchozího vidění pomocí H-Beta filtru. Části jižně od pásu jsme překvapivě neviděli ani na La Palme (pravděpodobně mají jiné emisní vlastnosti a není vhodný H-Beta filtr). + +Dominik: Jedno úspěšné pozorování u Pavouka na Cerové mi vyvrátilo řeči, že tento objekt je obtížné pozorovat. Na tento objekt jsem se velmi těšil, protože jsem o něm vždy jen slyšel mluvit a četl jsem o něm reporty, které většinou hovořily o náročnosti pozorování tohoto objektu. Avšak náročnost se mi nepotvrdila, Pavouk mi nastavil oblouk do zorného pole s H-beta filtrem a já jsem se jen divil. Byl to jasný šedý pás přes zorné pole, žádná nenápadná změna kontrastu, ale normální jasný oblak. Oblouk jsem si mohl pohybováním dalekohledu podívat celý a je to pozoruhodný pohled! + + + diff --git a/cs/dso/UGC/UGC3573_600u800.md b/cs/dso/UGC/UGC3573_600u800.md index 0803364db..9320c3e29 100644 --- a/cs/dso/UGC/UGC3573_600u800.md +++ b/cs/dso/UGC/UGC3573_600u800.md @@ -4,7 +4,7 @@ rating: 5 created_by: skybber created_date: 2020-09-23 20:52:17.927341 updated_by: skybber -updated_date: 2020-11-17 18:41:20.657744 +updated_date: 2022-12-17 09:00:06.864239 --- -419x, 6m5+ -tvoří pár s CGCG 145-17 UGC je okamžitě vidět v okuláru. Má velmi kompaktní, hvězdné a povrchově jasné jádro, které vypadá jako hvězda v popředí. Střední oblast kolem světelného jádra je mírně protáhlá, extrémní poměr os, žádná vyduť. \ No newline at end of file +419x, 6m5+ +tvoří pár s CGCG 145-17 UGC je okamžitě viditelná. Má velmi kompaktní, stelárrní a jasné jádro, které vypadá jako hvězda v popředí. Střední oblast kolem jasného jádra je mírně protáhlá, extrémní poměr os, žádná vyduť. \ No newline at end of file diff --git a/cs/star/Dunlop_236.md b/cs/star/Dunlop_236.md index db6efdbb7..e589d9e7e 100644 --- a/cs/star/Dunlop_236.md +++ b/cs/star/Dunlop_236.md @@ -3,7 +3,7 @@ name: Dunlop 236 constellation: Mic created_by: editor.cs created_date: 2020-09-23 20:52:21.784834 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:21.784855 +updated_by: skybber +updated_date: 2022-12-29 11:46:35.735874 --- -nádherný široký pár (57,4 ") dvou téměř stejně jasných hvězd (6,5mag a 6,9mag) vhodný pro binární a malé dalekohledy. \ No newline at end of file +nádherný široký pár (57,4") dvou téměř stejně jasných hvězd (6,5mag a 6,9mag) vhodný pro binární a malé dalekohledy. \ No newline at end of file diff --git a/cs/star/hr1175.md b/cs/star/hr1175.md index 921f514f7..70efe4586 100644 --- a/cs/star/hr1175.md +++ b/cs/star/hr1175.md @@ -3,7 +3,7 @@ name: β Ret constellation: Ret created_by: editor.cs created_date: 2020-09-23 20:52:23.530524 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:23.530562 +updated_by: skybber +updated_date: 2023-01-03 17:10:22.429462 --- -hlavní složka má jasnost 3,85mag a ve vzdálenosti 14 "se nachází její průvodce s magnitudě 8,1mag. Leží ve vzdálenosti 100 světelných let. \ No newline at end of file +hlavní složka má jasnost 3,85mag a ve vzdálenosti 14" se nachází její průvodce s magnitudě 8,1mag. Leží ve vzdálenosti 100 světelných let. \ No newline at end of file diff --git a/cs/star/hr1336.md b/cs/star/hr1336.md index 0433c8a7c..aacc52735 100644 --- a/cs/star/hr1336.md +++ b/cs/star/hr1336.md @@ -4,6 +4,6 @@ constellation: Ret created_by: editor.cs created_date: 2020-09-23 20:52:23.662243 updated_by: skybber -updated_date: 2022-04-08 14:45:36.673109 +updated_date: 2023-01-03 17:10:09.486262 --- -nejjasnější hvězda souhvězdí zdánlivé jasnosti 3,36mag. Patří do spektrální třídy G6 a je slabě nažloutlá. V úhlové vzdálenosti 48,5 "se nachází průvodce 12mag. Vzdálená je 163 světelných let. \ No newline at end of file +nejjasnější hvězda souhvězdí zdánlivé jasnosti 3,36mag. Patří do spektrální třídy G6 a je slabě nažloutlá. V úhlové vzdálenosti 48,5" se nachází průvodce 12mag. Vzdálená je 163 světelných let. \ No newline at end of file diff --git a/cs/star/hr1355.md b/cs/star/hr1355.md index 52fb18729..f991d2080 100644 --- a/cs/star/hr1355.md +++ b/cs/star/hr1355.md @@ -3,7 +3,7 @@ name: ε Ret constellation: Ret created_by: editor.cs created_date: 2020-09-23 20:52:22.121627 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:22.121646 +updated_by: skybber +updated_date: 2023-01-03 17:10:32.249652 --- -dvojhvězda tvořena hlavní složkou jasnosti 4,4mag a slabým průvodcem 12,5mag, který leží v odstupu 13,7 ". Systém leží ve vzdálenosti 60 světelných let. \ No newline at end of file +dvojhvězda tvořena hlavní složkou jasnosti 4,4mag a slabým průvodcem 12,5mag, který leží v odstupu 13,7". Systém leží ve vzdálenosti 60 světelných let. \ No newline at end of file diff --git a/cs/star/hr1605.md b/cs/star/hr1605.md index a2b7f3d66..94d2c5819 100644 --- a/cs/star/hr1605.md +++ b/cs/star/hr1605.md @@ -4,6 +4,6 @@ constellation: Aur created_by: editor.cs created_date: 2020-09-23 20:52:21.400663 updated_by: skybber -updated_date: 2020-09-23 20:52:21.400684 +updated_date: 2022-12-03 20:44:06.982874 --- -jedna ze tří hvězd kůzlat, která patří mezi pozoruhodné zákrytové proměnné hvězdy typu Algol. Sestává z jasného bílého veleobra s průměrem 4 miliard km, 37 000krát svítivějšího než Slunce a tmavého průvodce, vizuálně však nepozorovatelný. Obě hvězdy jsou ve vzájemném oběhu. Každých 27 let - 9 883 dní - se tmavá složka dostane před veleobra a zastíní velkou část jeho světla, čímž nám hvězda ε Aur na obloze výrazně ztmavne - z 3,1mag na 3,8mag. Toto potemnělé trvá celé měsíce - asi 190 dní, pak hvězda setrvá asi půl roku v minimu, a za dalších 190 dnů naroste z minima na maximum. To naznačuje, že průvodce musí být obklopen tmavým mrakem plynu a prachu. Poslední takový zákryt nastal v roce 2009. Mezi známými zákrytovými proměnnými vykazuje jednu z nejdelších period. \ No newline at end of file +jedna ze tří hvězd kůzlat, která patří mezi pozoruhodné zákrytové proměnné hvězdy typu Algol. Sestává z jasného bílého veleobra, 37 000krát svítivějšího než Slunce a tmavého průvodce, který však není vizuálně pozorovatelný. Obě hvězdy jsou ve vzájemném oběhu. Každých 27 let - 9 883 dní - se tmavá složka dostane před veleobra a zastíní velkou část jeho světla, čímž nám hvězda ε Aur na obloze výrazně ztmavne - z 3,1mag na 3,8mag. Toto potemnělé trvá celé měsíce - asi 190 dní, pak hvězda setrvá asi půl roku v minimu, a za dalších 190 dnů naroste z minima na maximum. To naznačuje, že průvodce musí být obklopen tmavým mrakem plynu a prachu. Poslední takový zákryt nastal v roce 2009. Mezi známými zákrytovými proměnnými vykazuje jednu z nejdelších period. \ No newline at end of file diff --git a/cs/star/hr183.md b/cs/star/hr183.md index 25c944378..6997641c7 100644 --- a/cs/star/hr183.md +++ b/cs/star/hr183.md @@ -3,7 +3,7 @@ name: ξ Phe constellation: Phe created_by: editor.cs created_date: 2020-09-23 20:52:22.266414 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:22.266433 +updated_by: skybber +updated_date: 2023-01-02 17:06:57.337772 --- -dobře rozlišitelná dvojhvězda pro dalekohled s průměrem objektivu kolem 100 mm. Hlavní složka má jasnost 6mag, průvodce v odstupu 13,2 "zase 10mag. \ No newline at end of file +dobře rozlišitelná dvojhvězda pro dalekohled s průměrem objektivu kolem 100 mm. Hlavní složka má jasnost 6mag, průvodce v odstupu 13,2" zase 10mag. \ No newline at end of file diff --git a/cs/star/hr191.md b/cs/star/hr191.md index a238c3f92..a29372fb9 100644 --- a/cs/star/hr191.md +++ b/cs/star/hr191.md @@ -3,7 +3,7 @@ name: η Phe constellation: Phe created_by: editor.cs created_date: 2020-09-23 20:52:23.773046 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:23.773081 +updated_by: skybber +updated_date: 2023-01-02 17:07:08.760073 --- -dvojhvězda, jejíž složky rozdílné jasnosti leží v odstupu 19,8 ". Jasnější dosahuje 4,5mag, průvodce vykazuje 11. hvězdnou velikost. \ No newline at end of file +dvojhvězda, jejíž složky rozdílné jasnosti leží v odstupu 19,8". Jasnější dosahuje 4,5mag, průvodce vykazuje 11. hvězdnou velikost. \ No newline at end of file diff --git a/cs/star/hr2020.md b/cs/star/hr2020.md index f08e821ad..d66d46b66 100644 --- a/cs/star/hr2020.md +++ b/cs/star/hr2020.md @@ -3,7 +3,7 @@ name: β Pic constellation: Pic created_by: editor.cs created_date: 2020-09-23 20:52:21.027117 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:21.027153 +updated_by: skybber +updated_date: 2023-01-02 17:52:15.855761 --- -jedna z hvězd, u které se po záznamech družice IRAS z roku 1983 zjistilo, že je obklopena diskem chladné látky - zejména prachu a ledu. Ten byl později i vyfotografování z obsevatória v Las Campanas v Chile 2,5 metrovým reflektorem Irénée du Pond. Disk se skládá z podobné hmoty, jaká se vyskytuje při vzniku planet, a tudíž tato hvězda by mohla být vhodným středem rodící se planetární soustavy. Na druhé straně svítivostí převyšuje Slunce až 60krát. Leží ve vzdálenosti 78 světelných let. Na obloze svítí jako modrobílá stálice 4. magnitudy. \ No newline at end of file +jedna z hvězd, u které se po záznamech družice IRAS z roku 1983 zjistilo, že je obklopena diskem chladné látky - zejména prachu a ledu. Ten byl později i vyfotografováný z obsevatória v Las Campanas v Chile 2,5 metrovým reflektorem Irénée du Pond. Disk se skládá z podobné hmoty, jaká se vyskytuje při vzniku planet, a tudíž tato hvězda by mohla být vhodným středem rodící se planetární soustavy. Na druhé straně svítivostí převyšuje Slunce až 60krát. Leží ve vzdálenosti 78 světelných let. Na obloze svítí jako modrobílá stálice 4. magnitudy. \ No newline at end of file diff --git a/cs/star/hr3433.md b/cs/star/hr3433.md index 348932146..737a94f6d 100644 --- a/cs/star/hr3433.md +++ b/cs/star/hr3433.md @@ -3,7 +3,7 @@ name: ζ Pyx constellation: Pyx created_by: editor.cs created_date: 2020-09-23 20:52:21.957471 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:21.957494 +updated_by: skybber +updated_date: 2023-01-03 17:05:53.890854 --- -hlavní složka má jasnost 5,5mag a její průvodce jasnosti 10mag ve vzdálenosti 52,3 "rozeznáme dalekohledem s průměrem objektivu 8 cm. \ No newline at end of file +hlavní složka má jasnost 5,5mag a její průvodce jasnosti 10mag ve vzdálenosti 52,3" rozeznáme dalekohledem s průměrem objektivu 8 cm. \ No newline at end of file diff --git a/cs/star/hr3438.md b/cs/star/hr3438.md index 646d2f05d..e80c9c4fd 100644 --- a/cs/star/hr3438.md +++ b/cs/star/hr3438.md @@ -3,7 +3,7 @@ name: β Pyx constellation: Pyx created_by: editor.cs created_date: 2020-09-23 20:52:22.396246 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:22.396263 +updated_by: skybber +updated_date: 2023-01-03 17:03:16.026870 --- -žlutý veleobr spektrální třídy G5. Průvodce jasnosti 12,5mag se od něj nachází v úhlové vzdálenosti 12,6 ". \ No newline at end of file +žlutý veleobr spektrální třídy G5. Průvodce jasnosti 12,5mag se od něj nachází v úhlové vzdálenosti 12,6". \ No newline at end of file diff --git a/cs/star/hr3541.md b/cs/star/hr3541.md index 9c42196a3..06b9ad1f2 100644 --- a/cs/star/hr3541.md +++ b/cs/star/hr3541.md @@ -4,6 +4,6 @@ constellation: Cnc created_by: editor.cs created_date: 2020-09-23 20:52:23.715389 updated_by: skybber -updated_date: 2021-12-18 17:04:03.662895 +updated_date: 2022-12-04 09:27:09.371844 --- -proměnná hvězda s nápadným červeným odstínem mění magnitudu od 5,6 do 7,5mag přibližně za 195 dní, vhodná na sledování triedru. Nachází se v blízkosti hvězdy δ Cancri. \ No newline at end of file +proměnná hvězda s nápadným červeným odstínem mění magnitudu od 5,6 do 7,5mag přibližně za 195 dní, vhodná na sledování v triedru. Nachází se v blízkosti hvězdy δ Cancri. \ No newline at end of file diff --git a/cs/star/hr3628.md b/cs/star/hr3628.md index 85903b25b..e3278d808 100644 --- a/cs/star/hr3628.md +++ b/cs/star/hr3628.md @@ -3,7 +3,7 @@ name: κ Pyx constellation: Pyx created_by: editor.cs created_date: 2020-09-23 20:52:21.366488 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:21.366511 +updated_by: skybber +updated_date: 2023-01-03 17:05:14.732466 --- -dvojhvězda, u hlavní složce s jasností 4,8mag se v odstupu 2,1 obloukové vteřiny nachází průvodce 10. hvězdné velikosti. Budeme potřebovat dalekohled s průměrem objektivu alespoň 150 mm. \ No newline at end of file +dvojhvězda, vedle složky s jasností 4,8mag se v odstupu 2,1 obloukové vteřiny nachází průvodce 10. hvězdné velikosti. Budeme potřebovat dalekohled s průměrem objektivu alespoň 150 mm. \ No newline at end of file diff --git a/cs/star/hr3644.md b/cs/star/hr3644.md index 4b25bba42..ffba35867 100644 --- a/cs/star/hr3644.md +++ b/cs/star/hr3644.md @@ -3,7 +3,7 @@ name: ε Pyx constellation: Pyx created_by: editor.cs created_date: 2020-09-23 20:52:23.721025 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:23.721057 +updated_by: skybber +updated_date: 2023-01-03 17:06:15.608999 --- -pozoruhodná vícenásobná hvězda. Hlavní složka má jasnost 5,6mag a v odstupu 17,8 "spatříme dalekohledem s průměrem objektivu 60 mm průvodce s jasností 9,2mag. Větším dalekohledem můžeme v odstupu 0,3 "pozorovat ještě hvězdu 10. magnitudy. \ No newline at end of file +pozoruhodná vícenásobná hvězda. Hlavní složka má jasnost 5,6mag a v odstupu 17,8" spatříme dalekohledem s průměrem objektivu 60 mm průvodce s jasností 9,2mag. Větším dalekohledem můžeme v odstupu 0,3 "pozorovat ještě hvězdu 10. magnitudy. \ No newline at end of file diff --git a/cs/star/hr6072.md b/cs/star/hr6072.md index 4c211a2fc..6fbbebc3a 100644 --- a/cs/star/hr6072.md +++ b/cs/star/hr6072.md @@ -3,7 +3,7 @@ name: γ1 a γ2 Nor constellation: Nor created_by: editor.cs created_date: 2020-09-23 20:52:21.171368 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:21.171401 +updated_by: skybber +updated_date: 2022-12-31 17:11:54.743096 --- -γ2 Nor je při své zdánlivé jasnosti 4,14mag nejjasnější hvězdou souhvězdí. γ1 Nor s ní vytváří optickou dvojhvězdu, kterou lze rozlišit i pouhým okem. γ2 Nor je oranžovým obrem vzdáleným 130 světelných let, průvodce jasnosti 5mag je vysokožiarivým bílým nadobro, který leží od ní více než 100-krát dále. Při γ2 Nor můžeme navíc v dalekohledu v odstupu 45 "najít společníka 10mag. \ No newline at end of file +γ2 Nor je při své zdánlivé jasnosti 4,14mag nejjasnější hvězdou souhvězdí. γ1 Nor s ní vytváří optickou dvojhvězdu, kterou lze rozlišit i pouhým okem. γ2 Nor je oranžovým obrem vzdáleným 130 světelných let, průvodce jasnosti 5mag je svítivým bílým nadobrem, který leží od ní více než 100-krát dále. Při γ2 Nor můžeme navíc v dalekohledu v odstupu 45 "najít společníka 10mag. \ No newline at end of file diff --git a/cs/star/hr6115.md b/cs/star/hr6115.md index 60311946f..dd5ae39bc 100644 --- a/cs/star/hr6115.md +++ b/cs/star/hr6115.md @@ -3,7 +3,7 @@ name: ε Nor constellation: Nor created_by: editor.cs created_date: 2020-09-23 20:52:21.462001 -updated_by: editor.cs -updated_date: 2020-09-23 20:52:21.462023 +updated_by: skybber +updated_date: 2022-12-31 17:13:02.484970 --- -pěkná dvojhvězda tvořena složkami jasnými 4,8mag a 7,5mag, které leží v odstupu 22,8 ". Rozlišíme jejich iv malém dalekohledu. Obě složky jsou navíc spektroskopické dvojhvězdy. \ No newline at end of file +pěkná dvojhvězda tvořena složkami jasnými 4,8mag a 7,5mag, které leží v odstupu 22,8". Rozlišíme jejich iv malém dalekohledu. Obě složky jsou navíc spektroskopické dvojhvězdy. \ No newline at end of file diff --git a/en/constellation/antlia.md b/en/constellation/antlia.md index 546ea0365..378ffaa3b 100644 --- a/en/constellation/antlia.md +++ b/en/constellation/antlia.md @@ -3,8 +3,8 @@ name: Antlia created_by: skybber created_date: 2021-06-01 19:50:34.718966 updated_by: skybber -updated_date: 2022-01-17 18:20:15.520122 +updated_date: 2022-12-29 08:55:25.008399 --- -Antlia is a small and inconspicuous constellation of the southern sky with no brighter stars, lying south of the pattern break in the middle of Hydra's body, near the much more conspicuous constellations of Sails and Astern. Its northern part is visible in the evening sky in Central Europe from mid-April to June, low over the southern horizon. There is nothing distinctive or interesting in the constellation of the Antlia when viewed through a trident or small telescope. Although the constellation lies just outside the southern Milky Way, it contains no star clusters or nebulae. There are only a few faint galaxies, but none (with the exception of NGC 2997), is brighter than 11th magnitude. - -![<]($IMG_DIR/cons/Ant.png) +Antlia is a small and inconspicuous constellation of the southern sky with no brighter stars, lying south of the pattern break in the middle of Hydra's body, near the much more conspicuous constellations of Vela and Puppis. Its northern part is visible in the evening sky in Central Europe from mid-April to June, low over the southern horizon. There is nothing distinctive or interesting in the constellation of the Antlia when viewed through a binocular or small telescope. Although the constellation lies just outside the southern Milky Way, it contains no star clusters or nebulae. There are only a few faint galaxies, but none (with the exception of NGC 2997), is brighter than 11th magnitude. + +![<]($IMG_DIR/cons/Ant.png) diff --git a/en/constellation/apus.md b/en/constellation/apus.md index 539557b1c..66ea1479c 100644 --- a/en/constellation/apus.md +++ b/en/constellation/apus.md @@ -3,8 +3,8 @@ name: Apus created_by: skybber created_date: 2021-06-01 19:53:52.148678 updated_by: skybber -updated_date: 2022-01-17 18:20:43.794519 +updated_date: 2022-12-29 08:58:37.270896 --- -Apus is a faint small constellation near the south celestial pole, lying south below the circle, the Southern triangle and the Altar. It is not visible in our latitudes or from the southernmost shores of Europe. Just above the horizon it only begins to appear in equatorial regions. The constellation is formed by the triangle of its brightest stars: α, β and γ, etc. The brightest of these is α etc., a slightly yellowish star that reaches a brightness of 3.81mag. The constellation otherwise contains virtually no objects of interest. - +Apus is a faint small constellation near the south celestial pole, lying south below the circle, the Triangulum Australe and the Altar. It is not visible in our latitudes or from the southernmost shores of Europe. Just above the horizon it only begins to appear in equatorial regions. The constellation is formed by the triangle of its brightest stars: α, β and γ, etc. The brightest of these is α etc., a slightly yellowish star that reaches a brightness of 3.81mag. The constellation otherwise contains virtually no objects of interest. + ![<]($IMG_DIR/cons/Aps.png) \ No newline at end of file diff --git a/en/constellation/ara.md b/en/constellation/ara.md index 231e6bbc4..f1613261f 100644 --- a/en/constellation/ara.md +++ b/en/constellation/ara.md @@ -3,8 +3,8 @@ name: Ara created_by: skybber created_date: 2021-06-01 20:13:42.313212 updated_by: skybber -updated_date: 2022-01-17 18:21:43.721601 +updated_date: 2022-12-29 09:00:03.117422 --- -A small but quite prominent constellation in the southern sky, not visible here. It lies in the Milky Way south of the constellation Scorpius, between the star θ Scorpii on one side and α Triangulo Australis on the other. Also pointing towards it are the two brightest Centaur stars, Hadar and Rigil Centaurus. The constellation Altar is quite distinctive in shape and resembles a chair or armchair in its outline in the sky. It can easily be found in the Milky Way south of Scorpio, however, if we can see at least to the 65th parallel of the southern declination from our vantage point. It consists of the brightest star β Arae of apparent brightness 2.85mag, an orange giant 600 light years away, followed by α Arae of brightness 2.95mag, γ Arae of 3.34mag, ζ Arae of 3.13mag, δ Arae of 3.62mag, θ Arae of 3.66mag, and η Arae of 3.76mag. Three of them are orange - β, ζ, η. The altar contains several interesting deep-sky objects, dominated by the globular clusters NGC 6352, NGC 6362 and NGC 6397 and the open cluster NGC 6208, which reaches stellar size 7. - +A small but quite prominent constellation in the southern sky, not visible here. It lies in the Milky Way south of the constellation Scorpius, between the star θ Scorpii on one side and α Triangulum Australe on the other. Also pointing towards it are the two brightest Centaur stars, Hadar and Rigil Centaurus. The constellation Altar is quite distinctive in shape and resembles a chair or armchair in its outline in the sky. It can easily be found in the Milky Way south of Scorpio, however, if we can see at least to the 65th parallel of the southern declination from our vantage point. It consists of the brightest star β Arae of apparent brightness 2.85mag, an orange giant 600 light years away, followed by α Arae of brightness 2.95mag, γ Arae of 3.34mag, ζ Arae of 3.13mag, δ Arae of 3.62mag, θ Arae of 3.66mag, and η Arae of 3.76mag. Three of them are orange - β, ζ, η. The altar contains several interesting deep-sky objects, dominated by the globular clusters NGC 6352, NGC 6362 and NGC 6397 and the open cluster NGC 6208, which reaches stellar size 7. + ![<]($IMG_DIR/cons/Ara.png) \ No newline at end of file diff --git a/en/constellation/auriga.md b/en/constellation/auriga.md index 2270158e7..e1ef9a93b 100644 --- a/en/constellation/auriga.md +++ b/en/constellation/auriga.md @@ -3,8 +3,8 @@ name: Auriga created_by: skybber created_date: 2021-06-02 18:57:03.133087 updated_by: skybber -updated_date: 2022-02-11 17:00:05.583123 +updated_date: 2023-01-06 17:04:00.585253 --- -A striking constellation in the northern sky in an interesting part of the winter Milky Way. Bright stars form a distinctive horseshoe pattern between the constellations Gemini and Perseus. Its northern part is circumpolar in our latitudes, the whole constellation not falling below the northern horizon until 60 degrees north latitude. The constellation of Auriga is easily found thanks to the bright star Capella, which is also accompanied a little further south by three stars: ε, ζ and η Aurigae, which are called "Kids of the she-goat Capella" (Haedus). They are visible as a small triangle of stars. It is at this point that the Milky Way begins to regain its brightness and continues next to the Ladder (a striking line of tight 5th magnitude constellations 16, 17, 18, 19 and IQ Aurigae) in the form of an interesting narrow band to the south. Within the distinctive horseshoe pattern formed by the constellation's five brightest stars lies the so-called Big Three in the Wozze - a trio of Messier clusters M36, M37 and M38, all of which can be visible without binoculars during excellent conditions. - +A striking constellation in the northern sky in an interesting part of the winter Milky Way. Bright stars form a distinctive horseshoe pattern between the constellations Gemini and Perseus. Its northern part is circumpolar in our latitudes, the whole constellation not falling below the northern horizon until 60 degrees north latitude. The constellation of Auriga is easily found thanks to the bright star Capella, which is also accompanied a little further south by three stars: ε, ζ and η Aurigae, which are called "Kids of the she-goat Capella" (Haedus). They are visible as a small triangle of stars. It is at this point that the Milky Way begins to regain its brightness and continues next to the Ladder (a striking line of tight 5th magnitude constellations 16, 17, 18, 19 and IQ Aurigae) in the form of an interesting narrow band to the south. Within the distinctive horseshoe pattern formed by the constellation's five brightest stars lies the so-called Big Three in the Auriga - a trio of Messier clusters M36, M37 and M38, all of which can be visible without binoculars during excellent conditions. + ![<]($IMG_DIR/cons/Aur.png) \ No newline at end of file diff --git a/en/constellation/cancer.md b/en/constellation/cancer.md index cc45df1e4..64c3abf27 100644 --- a/en/constellation/cancer.md +++ b/en/constellation/cancer.md @@ -3,8 +3,8 @@ name: Cancer created_by: skybber created_date: 2021-06-02 19:22:26.823362 updated_by: skybber -updated_date: 2022-02-11 18:34:48.842625 +updated_date: 2023-01-06 17:05:57.408081 --- -A faint constellation in the northern sky between Gemini and Leo. The inverted "Y" lies in the centre of an equilateral triangle formed by the stars Pollux, Regulus and Procyon. It is formed by the stars Altarf, Acubens, Asellus Australus, ι and χ Cancri. 2000 years ago, the Sun passed through Cancer at the time of the summer solstice, so it was the northernmost constellation of the zodiac. It currently passes through it from July 20 to August 9. However, the sign of Cancer still marks the summer solstice and the Tropic of Cancer is called the Tropic of Cancer in the northern hemisphere. At present, the Sun rises highest in the northern hemisphere at the boundary of the constellations Gemini and Taurus. Cancer is the least prominent constellation of the zodiac, with only one of its stars exceeding 4th magnitude. A moonless night is therefore a prerequisite for seeing the constellation at its best in the sky. Cancer boasts two open star clusters, some of the most beautiful in the entire sky. The brighter one is M44, located almost in the centre of the constellation. In ancient times, in 270 BC, the Greek poet Aratus called it "Praesepe". Several centuries have passed since then, when Galileo Galilei first resolved them into individual stars with a telescope in 1610. Nowadays, a simple binocular will do the trick. There are also several binary stars in the constellation, and because it is further away from the Milky Way, we can find a greater number of fainter galaxies. - +A faint constellation in the northern sky between Gemini and Leo. The inverted "Y" lies in the centre of an equilateral triangle formed by the stars Pollux, Regulus and Procyon. It is formed by the stars Altarf, Acubens, Asellus Australus, ι and χ Cancri. 2000 years ago, the Sun passed through Cancer at the time of the summer solstice, so it was the northernmost constellation of the zodiac. It currently passes through it from July 20 to August 9. However, the sign of Cancer still marks the summer solstice and the tropic is called the Tropic of Cancer in the northern hemisphere. At present, the Sun rises highest in the northern hemisphere at the boundary of the constellations Gemini and Taurus. Cancer is the least prominent constellation of the zodiac, with only one of its stars exceeding 4th magnitude. A moonless night is therefore a prerequisite for seeing the constellation at its best in the sky. Cancer boasts two open star clusters, some of the most beautiful in the entire sky. The brighter one is M44, located almost in the centre of the constellation. In ancient times, in 270 BC, the Greek poet Aratus called it "Praesepe". Several centuries have passed since then, when Galileo Galilei first resolved them into individual stars with a telescope in 1610. Nowadays, a simple binocular will do the trick. There are also several binary stars in the constellation, and because it is further away from the Milky Way, we can find a greater number of fainter galaxies. + ![<]($IMG_DIR/cons/Cnc.png) \ No newline at end of file diff --git a/en/constellation/canis major.md b/en/constellation/canis major.md index 288951ff3..bacf045b1 100644 --- a/en/constellation/canis major.md +++ b/en/constellation/canis major.md @@ -3,8 +3,8 @@ name: Canis Major created_by: skybber created_date: 2021-06-03 15:40:18.970565 updated_by: skybber -updated_date: 2022-02-12 08:57:08.003621 +updated_date: 2023-01-06 17:41:14.860699 --- -A striking constellation in the southern sky, made up of bright and simply arranged stars. The constellation includes Sirius, the brightest star in the night sky. Apart from the Sun and the Moon, it is only outshined by the planets Jupiter, Saturn and Mars. Sirius is also one of the vertices of the Winter Triangle, along with Procyon of the Canis Major and the star Betelgeuse in the right arm of Orion. The constellation is not the most extensive, but neither is it somehow poor in interesting objects that become the target of many amateur astronomers. Thanks to its position in the Milky Way's winter Milky Way, the Big Dog is rich in various open clusters, of which M41 is the clear leader. It also contains several nebula complexes, a planetary nebula, and a few galaxies whose light has broken through the gas and dust clouds of the Milky Way. For binary enthusiasts, this rich region is certainly well suited. Globular clusters are not found in the constellation. - +A striking constellation in the southern sky, made up of bright and simply arranged stars. The constellation includes Sirius, the brightest star in the night sky. Apart from the Sun and the Moon, it is only outshined by the planets Jupiter, Saturn and Mars. Sirius is also one of the vertices of the Winter Triangle, along with Procyon of the Canis Major and the star Betelgeuse in the right arm of Orion. The constellation is not the most extensive, but neither is it somehow poor in interesting objects that become the target of many amateur astronomers. Thanks to its position in the Milky Way's winter Milky Way, the Canis Major is rich in various open clusters, of which M41 is the clear leader. It also contains several nebula complexes, a planetary nebula, and a few galaxies whose light has broken through the gas and dust clouds of the Milky Way. For binary enthusiasts, this rich region is certainly well suited. Globular clusters are not found in the constellation. + ![<]($IMG_DIR/cons/CMa.png) \ No newline at end of file diff --git a/en/constellation/canis minor.md b/en/constellation/canis minor.md index 5da580398..78e5d5e4d 100644 --- a/en/constellation/canis minor.md +++ b/en/constellation/canis minor.md @@ -3,8 +3,8 @@ name: Canis Minor created_by: skybber created_date: 2021-06-03 15:42:44.019373 updated_by: skybber -updated_date: 2022-02-12 08:57:27.803601 +updated_date: 2023-01-06 17:52:03.371165 --- -A small constellation of the northern sky near the celestial equator, below Gemini and east of Orion, containing only two stars brighter than 5 magnitude: Procyon and Gomeisa. Although located on the edge of the winter Milky Way, Little Dog offers the observer only a few faint galaxies from deepsky objects, nothing for smaller telescopes. Even binaries are not well represented, but a few are interesting and attention-grabbing. Quasar 4C 05.34, which is one of the most distant objects in the sky at 3,000 Mpc, also lies in the constellation. - +A small constellation of the northern sky near the celestial equator, below Gemini and east of Orion, containing only two stars brighter than 5 magnitude: Procyon and Gomeisa. Although located on the edge of the winter Milky Way, Canis Minor offers the observer only a few faint galaxies from deepsky objects, nothing for smaller telescopes. Even binaries are not well represented, but a few are interesting and attention-grabbing. Quasar 4C 05.34, which is one of the most distant object in the sky at 3,000 Mpc, also lies in the constellation. + ![<]($IMG_DIR/cons/CMi.png) \ No newline at end of file diff --git a/en/constellation/carina.md b/en/constellation/carina.md index d7d3d718c..b7686be3b 100644 --- a/en/constellation/carina.md +++ b/en/constellation/carina.md @@ -3,9 +3,9 @@ name: Carina created_by: skybber created_date: 2021-06-06 08:40:05.845624 updated_by: skybber -updated_date: 2022-02-11 18:35:07.098423 +updated_date: 2022-12-29 09:07:40.160818 --- -![<]($IMG_DIR/cons/Car.png) -Keel is the dominant constellation in the southern sky, with the entire eastern part of the constellation delving into one of the richest regions of the Milky Way, with an extensive array of deep-sky objects. Six bright open clusters can be found here in binocular alone. Three of them are real showpieces: NGC 2516 and NGC 3532 are very bright, large and contain many stars. IC 2602 is a group of other bright stars popularly known as the Southern Pleiades. The second brightest star in the sky, Canopus, and the η Carinae Nebula, the brightest region of ionized hydrogen in the Milky Way, occupy an area of four degrees in the sky. In its interior lies a very interesting 6th magnitude star, also called η Carinae. It is a pity that the constellation of the keel is practically impossible to observe from Europe. - -Of particular note here is the bright and sharply defined Milky Way cloud, which spills over into the neighbouring Southern Cross. Of all the parts of the Milky Way, it appears the most colourful - white, with a very slight tendency to a bluish hue. It is important to note that at this point our view turns directly along the axis of Sagittarius' spiral arm. You can trace its northeastern part all the way to the constellation of the Shield, where it bends again at the point of the Cloud in the Shield. However, if you look more closely you will see that while the Cloud in the Shield is only 25 degrees from the centre of the Galaxy, the star cloud in Kyle is a good 75 degrees away. The explanation is simple. The arm of Sagittarius starts from the centre of the Galaxy in the direction of the constellation of the Shield and stretches further south, while in Kyle it is already far from it, encircling the centre and disappearing in the distance behind it. While objects in Sagittarius are on average five thousand light-years away, NGC 6231 in Scorpius is already 6,000 light-years away and NGC 4755 in the Southern Cross is 8,000 light-years away. Within the star cloud itself, there are a couple of diverse subdivisions that look like dark smudges in binoculars over a very rich star field surrounding several of the aforementioned clusters. A truly unique sight. +![<]($IMG_DIR/cons/Car.png) +Carina is the dominant constellation in the southern sky, with the entire eastern part of the constellation delving into one of the richest regions of the Milky Way, with an extensive array of deep-sky objects. Six bright open clusters can be found here in binocular alone. Three of them are real showpieces: NGC 2516 and NGC 3532 are very bright, large and contain many stars. IC 2602 is a group of other bright stars popularly known as the Southern Pleiades. The second brightest star in the sky, Canopus, and the η Carinae Nebula, the brightest region of ionized hydrogen in the Milky Way, occupy an area of four degrees in the sky. In its interior lies a very interesting 6th magnitude star, also called η Carinae. It is a pity that the constellation of the Carina is practically impossible to observe from Europe. + +Of particular note here is the bright and sharply defined Milky Way cloud, which spills over into the neighbouring Crux. Of all the parts of the Milky Way, it appears the most colourful - white, with a very slight tendency to a bluish hue. It is important to note that at this point our view turns directly along the axis of Sagittarius' spiral arm. You can trace its northeastern part all the way to the constellation of the Scutum, where it bends again at the point of the Cloud in the Scutum. However, if you look more closely you will see that while the Cloud in the Scutum is only 25 degrees from the centre of the Galaxy, the star cloud in Carina is a good 75 degrees away. The explanation is simple. The arm of Sagittarius starts from the centre of the Galaxy in the direction of the constellation of the Scutum and stretches further south, while in Carina it is already far from it, encircling the centre and disappearing in the distance behind it. While objects in Sagittarius are on average five thousand light-years away, NGC 6231 in Scorpius is already 6,000 light-years away and NGC 4755 in the Southern Cross is 8,000 light-years away. Within the star cloud itself, there are a couple of diverse subdivisions that look like dark smudges in binoculars over a very rich star field surrounding several of the aforementioned clusters. A truly unique sight. diff --git a/en/constellation/centaurus.md b/en/constellation/centaurus.md index bef856cf4..681b9f83f 100644 --- a/en/constellation/centaurus.md +++ b/en/constellation/centaurus.md @@ -3,9 +3,9 @@ name: Centaurus created_by: skybber created_date: 2021-06-06 08:43:12.898913 updated_by: skybber -updated_date: 2022-02-11 18:35:44.997565 +updated_date: 2022-12-29 09:14:22.879062 --- -![<]($IMG_DIR/cons/Cen.png) -A large, striking and object-rich constellation in the southern sky, the northern parts of which are still visible from central Europe in the spring months. The constellation's two brightest stars - α Centauri, also called Toliman or Rigil Centaurus - and β Centauri - Agena or Hadar - form the centaur's legs and are also a landmark for locating the South Celestial Pole and the Southern Cross. The latter was still part of the Centaurus in Ptolemy's time, only later becoming a separate constellation. Unfortunately, these regions are now too far south and cannot be seen from Europe. A rich Milky Way region passes through the southern part of the constellation and therefore, especially in its central and eastern part towards the Wolf Interface, we can observe several nice open clusters. By far the most famous object, however, is the impressive globular cluster Omega Centauri, the brightest in the entire sky. Also worth noting is the large and bright galaxy NGC 5128 in the center with its dark band, one of the strongest radio sources in the sky. - -South of λ Centauri lies a dark nebula, called the False Coal Bag by southern observers, at the boundary between Centaurus, the keel and the Fly. While not as conspicuous by comparison because of a few foreground stars, it is considerably larger. Its contrast to its surroundings is not quite as stark, yet it is clearly visible compared to the Milky Way. The beautiful cluster Melotte 115, which consists of many faint stars, also appears in the binocular near it. Near Alpha Centauri, a complex of dark clouds called the Trench begins, dividing the Milky Way in two. It gradually grows in width and continues to the centre of the Galaxy, because the beginning of the galaxy at Alpha Centauri is further away than the other end, so it is also narrower and more sharply defined at this point. +![<]($IMG_DIR/cons/Cen.png) +A large, striking and object-rich constellation in the southern sky, the northern parts of which are still visible from central Europe in the spring months. The constellation's two brightest stars - α Centauri, also called Toliman or Rigil Centaurus - and β Centauri - Agena or Hadar - form the centaur's legs and are also a landmark for locating the South Celestial Pole and the Crux. The latter was still part of the Centaurus in Ptolemy's time, only later becoming a separate constellation. Unfortunately, these regions are now too far south and cannot be seen from Europe. A rich Milky Way region passes through the southern part of the constellation and therefore, especially in its central and eastern part towards the borders of Lupus, we can observe several nice open clusters. By far the most famous object, however, is the impressive globular cluster Omega Centauri, the brightest in the entire sky. Also worth noting is the large and bright galaxy NGC 5128 in the center with its dark band, one of the strongest radio sources in the sky. + +South of λ Centauri lies a dark nebula, called the False Coal Cack by southern observers, at the boundary between Centaurus, the Centaurus and the Musca. While not as conspicuous by comparison because of a few foreground stars, it is considerably larger. Its contrast to its surroundings is not quite as stark, yet it is clearly visible compared to the Milky Way. The beautiful cluster Melotte 115, which consists of many faint stars, also appears in the binocular near it. Near Alpha Centauri, a complex of dark clouds called the Trench begins, dividing the Milky Way in two. It gradually grows in width and continues to the centre of the Galaxy, because the beginning of the galaxy at Alpha Centauri is further away than the other end, so it is also narrower and more sharply defined at this point. diff --git a/en/constellation/chamaeleon.md b/en/constellation/chamaeleon.md index a0f88e150..210309f5f 100644 --- a/en/constellation/chamaeleon.md +++ b/en/constellation/chamaeleon.md @@ -3,7 +3,7 @@ name: Chamaeleon created_by: skybber created_date: 2021-06-06 08:46:38.987686 updated_by: skybber -updated_date: 2022-01-17 18:27:06.695571 +updated_date: 2022-12-29 09:19:56.022358 --- -![<]($IMG_DIR/cons/Cha.png) -A tiny constellation near the south celestial pole forming an inconspicuous irregular rhombus of stars of apparent brightness 4mag and 5mag south of the flying fish, the keel and the Fly. Its defining stars are α, β, γ and δ Chamaeleontis. Chameleon is, as in nature, inconspicuous in the sky: it disappears in a region poor in brighter stars around the south celestial pole. All the stars of Chameleon are faint, and the constellation is one of the smallest and most difficult to identify. It is only revealed by the longer arm of the Southern Cross pointing at it from the north. The constellation is not visible to us. \ No newline at end of file +![<]($IMG_DIR/cons/Cha.png) +A tiny constellation near the south celestial pole forming an inconspicuous irregular rhombus of stars of apparent brightness 4mag and 5mag south of the flying fish, the Centaurus and the Musca. Its defining stars are α, β, γ and δ Chamaeleontis. Chameleon is, as in nature, inconspicuous in the sky: it disappears in a region poor in brighter stars around the south celestial pole. All the stars of Chameleon are faint, and the constellation is one of the smallest and most difficult to identify. It is only revealed by the longer arm of the Southern Cross pointing at it from the north. The constellation is not visible to us. \ No newline at end of file diff --git a/en/constellation/circinus.md b/en/constellation/circinus.md index 10fe002af..935b1bb2f 100644 --- a/en/constellation/circinus.md +++ b/en/constellation/circinus.md @@ -3,9 +3,9 @@ name: Circinus created_by: skybber created_date: 2021-06-06 08:47:29.607575 updated_by: skybber -updated_date: 2022-02-11 18:15:24.808230 +updated_date: 2022-12-29 09:23:46.432952 --- -![<]($IMG_DIR/cons/Cir.png) -A small and faint constellation of the southern sky that we can never see in our latitudes. The narrow isosceles triangle formed by the constellation's three brightest stars lies wedged between the Fly, Centaurus, Ruler and the Southern Triangle in the Milky Way. There are no interesting objects in this small constellation near the conspicuous α and β Centauri, despite lying in the Milky Way, and its faint stars are not even named. - -At positions 14 47.8 (RA) and -66 17 (Dec), you can discover the South Kemble Cascade, a purely random grouping of individual constellations in the constellation of the circle in binocular. However, in comparison to the original, it is slightly shorter and contains up to two streams of stars that merge in the north. More striking is the straight, forty-five minute long western array consisting of eight stars. The eastern row contains the same number of stars, but is a little twisted, and its brightest star is Dzetou Circinus. The other joining stars in the south give the whole cluster a necklace-like appearance. +![<]($IMG_DIR/cons/Cir.png) +A small and faint constellation of the southern sky that we can never see in our latitudes. The narrow isosceles triangle formed by the constellation's three brightest stars lies wedged between the Musca, Centaurus, Norma and the Triangulum Australis in the Milky Way. There are no interesting objects in this small constellation near the conspicuous α and β Centauri, despite lying in the Milky Way, and its faint stars are not even named. + +At positions 14 47.8 (RA) and -66 17 (Dec), you can discover the South Kemble Cascade, a purely random grouping of individual constellations in the constellation of the circle in binocular. However, in comparison to the original, it is slightly shorter and contains up to two streams of stars that merge in the north. More striking is the straight, forty-five minute long western array consisting of eight stars. The eastern row contains the same number of stars, but is a little twisted, and its brightest star is Dzeta Circinus. The other joining stars in the south give the whole cluster a necklace-like appearance. diff --git a/en/constellation/columba.md b/en/constellation/columba.md index dba390c40..1c72d1a71 100644 --- a/en/constellation/columba.md +++ b/en/constellation/columba.md @@ -3,7 +3,7 @@ name: Columba created_by: skybber created_date: 2021-06-06 08:48:45.613176 updated_by: skybber -updated_date: 2022-01-17 18:27:35.545760 +updated_date: 2022-12-29 08:54:01.844904 --- -![<]($IMG_DIR/cons/Col.png) -A small constellation of the southern sky, whose distorted line of stars lies south of the Big Dog and Hare. Dove can be seen all above the horizon from areas as far south as the southernmost European shores. If we want the best view of its objects, we must wait for a time when it is passing through the meridian and the southern horizon is not obscured by fog, dust, or low cloud. The Dove contains a handful of binaries, a couple of moderately bright galaxies, and the pretty globular cluster NGC 1851. +![<]($IMG_DIR/cons/Col.png) +A small constellation of the southern sky, whose distorted line of stars lies south of the Canis Major and Lepus. Columba can be seen all above the horizon from areas as far south as the southernmost European shores. If we want the best view of its objects, we must wait for a time when it is passing through the meridian and the southern horizon is not obscured by fog, dust, or low cloud. The Columba contains a handful of binaries, a couple of moderately bright galaxies, and the pretty globular cluster NGC 1851. diff --git a/en/constellation/dorado.md b/en/constellation/dorado.md index a61b2a9f5..d1dec826d 100644 --- a/en/constellation/dorado.md +++ b/en/constellation/dorado.md @@ -3,7 +3,7 @@ name: Dorado created_by: skybber created_date: 2021-06-20 18:25:05.532409 updated_by: skybber -updated_date: 2021-06-20 18:25:05.532777 +updated_date: 2022-12-29 10:03:36.105342 --- -![<]($IMG_DIR/cons/Dor.png) -A faint and minor constellation of the southern sky south of Malir, not rising in our area. The essentially inconspicuous region lies between the bright stars Canopus and Achernar. There is only one star brighter than fourth magnitude. However, if we look closely, we can see a bright white cloud on the boundary of the constellation with Table Mountain - the Large Magellanic Cloud. The constellation also contains the south pole of the ecliptic. +![<]($IMG_DIR/cons/Dor.png) +A faint and minor constellation of the southern sky south of Pictor, not rising in our area. The essentially inconspicuous region lies between the bright stars Canopus and Achernar. There is only one star brighter than fourth magnitude. However, if we look closely, we can see a bright white cloud on the boundary of the constellation with Table Mountain - the Large Magellanic Cloud. The constellation also contains the south pole of the ecliptic. diff --git a/en/constellation/grus.md b/en/constellation/grus.md index bc4601e7a..841a7b8ac 100644 --- a/en/constellation/grus.md +++ b/en/constellation/grus.md @@ -3,7 +3,7 @@ name: Grus created_by: skybber created_date: 2021-06-26 08:44:02.032917 updated_by: skybber -updated_date: 2021-06-26 08:44:02.033163 +updated_date: 2022-12-29 10:12:53.309408 --- -![<]($IMG_DIR/cons/Gru.png) -A fairly prominent constellation of the southern sky in the shape of an inverted cross, below the bright Fomalhaut of the Southern Fish. With a little imagination in the distribution of the stars, we can see a flying crane with its legs spread back, neck stretched out and head held high. Only the northernmost part is visible in our evening sky. For observers with smaller binoculars, apart from a few binaries, the constellation is poor in objects, although for instruments with binoculars with a lens diameter of around 200 mm it has some nice extragalactic objects. In the northeastern part of the constellation, north of the star θ Gruis, there is a small group of 10th to 11th magnitude galaxies, most of which are spiral galaxies: NGC 7410, 7424, 7552 and 7590. \ No newline at end of file +![<]($IMG_DIR/cons/Gru.png) +A fairly prominent constellation of the southern sky in the shape of an inverted cross, below the bright Fomalhaut of the Piscis Austrinus. With a little imagination in the distribution of the stars, we can see a flying crane with its legs spread back, neck stretched out and head held high. Only the northernmost part is visible in our evening sky. For observers with smaller binoculars, apart from a few binaries, the constellation is poor in objects, although for instruments with binoculars with a lens diameter of around 200 mm it has some nice extragalactic objects. In the northeastern part of the constellation, north of the star θ Gruis, there is a small group of 10th to 11th magnitude galaxies, most of which are spiral galaxies: NGC 7410, 7424, 7552 and 7590. \ No newline at end of file diff --git a/en/constellation/hydrus.md b/en/constellation/hydrus.md index 532a2e85c..711882a28 100644 --- a/en/constellation/hydrus.md +++ b/en/constellation/hydrus.md @@ -3,7 +3,7 @@ name: Hydrus created_by: skybber created_date: 2021-06-29 07:06:31.563419 updated_by: skybber -updated_date: 2021-06-29 07:06:31.563775 +updated_date: 2022-12-29 10:18:48.547589 --- -![<]($IMG_DIR/cons/Hyi.png) -A minor constellation near the south celestial pole, near Achernar of Eridania. It takes the form of an isosceles triangle that lies between the Large and Small Magellanic Clouds. The Water Serpent is not visible at our latitudes. \ No newline at end of file +![<]($IMG_DIR/cons/Hyi.png) +A minor constellation near the south celestial pole, near Achernar of Eridanus. It takes the form of an isosceles triangle that lies between the Large and Small Magellanic Clouds. The Hydrus is not visible at our latitudes. \ No newline at end of file diff --git a/en/constellation/indus.md b/en/constellation/indus.md index e76d7b305..3374dd34c 100644 --- a/en/constellation/indus.md +++ b/en/constellation/indus.md @@ -3,7 +3,7 @@ name: Indus created_by: skybber created_date: 2021-06-29 07:07:25.645155 updated_by: skybber -updated_date: 2021-06-29 07:07:25.645418 +updated_date: 2022-12-29 11:10:56.821293 --- -![<]($IMG_DIR/cons/Ind.png) -A small and faint constellation of the southern sky surrounded by a trio of feathered constellations: the Crane, the Toucan, the Peacock, and straying to near the south pole of the sky. It is probably difficult to imagine a North American Indian in the few obscure stars of this constellation. The slightly more conspicuous Peacock, whose brightest star, Peacock, lies in close proximity to the Indian, may serve as a guide to locating the constellation. This constellation is not visible here. +![<]($IMG_DIR/cons/Ind.png) +A small and faint constellation of the southern sky surrounded by a trio of feathered constellations: the Grus, the Tucana, the Pavo, and straying to near the south pole of the sky. It is probably difficult to imagine a North American Indian in the few obscure stars of this constellation. The slightly more conspicuous Pavo, whose brightest star, Pavo, lies in close proximity to the Indian, may serve as a guide to locating the constellation. This constellation is not visible here. diff --git a/en/constellation/mensa.md b/en/constellation/mensa.md index 9d351a216..a14079f98 100644 --- a/en/constellation/mensa.md +++ b/en/constellation/mensa.md @@ -3,7 +3,7 @@ name: Mensa created_by: skybber created_date: 2021-06-29 09:43:40.525334 updated_by: skybber -updated_date: 2021-06-29 09:43:40.525571 +updated_date: 2022-12-29 11:27:38.247053 --- -![<]($IMG_DIR/cons/Men.png) -A small and faint constellation in close proximity to the south pole of the sky, therefore not visible at our latitudes. Table Mountain is the faintest constellation in the sky, with the brightest stars not exceeding fifth magnitude. Four of them form the main pattern of the constellation. Of the objects of note, only the Great Magellanic Cloud is worth mentioning, which partially extends here from the neighbouring Mečiar to the north. +![<]($IMG_DIR/cons/Men.png) +A small and faint constellation in close proximity to the south pole of the sky, therefore not visible at our latitudes. The Mensa is the faintest constellation in the sky, with the brightest stars not exceeding fifth magnitude. Four of them form the main pattern of the constellation. Of the objects of note, only the Great Magellanic Cloud is worth mentioning, which partially extends here from the neighbouring Dorado to the north. diff --git a/en/constellation/microscopium.md b/en/constellation/microscopium.md index 7b04b7059..90f398be4 100644 --- a/en/constellation/microscopium.md +++ b/en/constellation/microscopium.md @@ -3,7 +3,7 @@ name: Microscopium created_by: skybber created_date: 2021-06-29 13:07:40.537565 updated_by: skybber -updated_date: 2021-06-29 13:07:40.537805 +updated_date: 2022-12-29 11:43:11.351455 --- -![<]($IMG_DIR/cons/Mic.png) -A small and faint constellation in the southern sky, a faint group of a few stars between the Southern Fish and Sagittarius, down below Capricorn. In our area, only its northern part rises above the horizon in late summer evenings. The microscope lies in a star-poor region of the sky, and none of its stars is brighter than 4.7mag. It contains no more than a few rather attractive binaries and a handful of faint galaxies. \ No newline at end of file +![<]($IMG_DIR/cons/Mic.png) +A small and faint constellation in the southern sky, a faint group of a few stars between the Piscis Austrinus and Sagittarius, down below Capricornus. In our area, only its northern part rises above the horizon in late summer evenings. The microscope lies in a star-poor region of the sky, and none of its stars is brighter than 4.7mag. It contains no more than a few rather attractive binaries and a handful of faint galaxies. \ No newline at end of file diff --git a/en/constellation/musca.md b/en/constellation/musca.md index 230ab29b8..3145bbdb6 100644 --- a/en/constellation/musca.md +++ b/en/constellation/musca.md @@ -3,7 +3,7 @@ name: Musca created_by: skybber created_date: 2021-06-29 13:12:26.974967 updated_by: skybber -updated_date: 2022-02-11 18:37:02.559791 +updated_date: 2022-12-31 15:34:58.764658 --- -![<]($IMG_DIR/cons/Mus.png) -A small constellation of the southern sky lying between the chameleons and the Southern Cross in the Milky Way, not visible from our latitudes. The constellation of the Fly is quite a striking feature, although apart from α muscae its stars do not exceed third magnitude. The star λ muscae is white and together with μ muscae, which is red, forms a contrasting pair in the binocular. Of the deep-sky objects in the constellation, two globular clusters that are visible to the binocular attract attention: NGC 4372 and NGC 4833, as well as a small portion of the dark Coal Sack Nebula that extends in from the neighboring Southern Cross. To the northwest of NGC 4372, there is again an interestingly curled dark filament a little bit of a degree in size - the Dark Doodad Nebula. \ No newline at end of file +![<]($IMG_DIR/cons/Mus.png) +A small constellation of the southern sky lying between the Chameleon and the Crux in the Milky Way, not visible from our latitudes. The constellation of the Musca is quite a striking feature, although apart from α Muscae its stars do not exceed third magnitude. The star λ Muscae is white and together with μ Muscae, which is red, forms a contrasting pair in the binocular. Of the deep-sky objects in the constellation, two globular clusters that are visible to the binocular attract attention: NGC 4372 and NGC 4833, as well as a small portion of the dark Coal Sack Nebula that extends in from the neighboring Crux. To the northwest of NGC 4372, there is again an interestingly curled dark filament a little bit of a degree in size - the Dark Doodad Nebula. \ No newline at end of file diff --git a/en/constellation/norma.md b/en/constellation/norma.md index e08b471cc..991a06a13 100644 --- a/en/constellation/norma.md +++ b/en/constellation/norma.md @@ -3,7 +3,7 @@ name: Norma created_by: skybber created_date: 2021-07-10 08:33:50.275312 updated_by: skybber -updated_date: 2022-02-11 18:16:24.481700 +updated_date: 2022-12-31 15:52:48.946300 --- -![<]($IMG_DIR/cons/Nor.png) -A small and fainter constellation of the southern sky that does not rise above the horizon at our latitudes. It lies along the galactic equator between the Wolf and the Altar in the region where the Milky Way is again split by the Great Rift. The constellation is located in a rich part of the Milky Way and is therefore a good destination for a binocular's walk across the sky. There is a striking star cloud here that is ivory white in colour. To the north of it, the Milky Way dissolves into an irregular and intricately complicated system interspersed with many brightenings and dark dust. The constellation's four brightest stars form a symmetrical trapezoid around which several open clusters are found. Two of them - NGC 6067 and 6087 - are usually visible as hazy patches without any optical aid. This small constellation is also lucky to have novae - one flared up here in 1893 and another appeared near here in 1920. \ No newline at end of file +![<]($IMG_DIR/cons/Nor.png) +A small and fainter constellation of the southern sky that does not rise above the horizon at our latitudes. It lies along the galactic equator between the Lupus and the Ara in the region where the Milky Way is again split by the Great Rift. The constellation is located in a rich part of the Milky Way and is therefore a good destination for a binocular's walk across the sky. There is a striking star cloud here that is ivory white in colour. To the north of it, the Milky Way dissolves into an irregular and intricately complicated system interspersed with many brightenings and dark dust. The constellation's four brightest stars form a symmetrical trapezoid around which several open clusters are found. Two of them - NGC 6067 and 6087 - are usually visible as hazy patches without any optical aid. This small constellation is also lucky to have novae - one flared up here in 1893 and another appeared near here in 1920. \ No newline at end of file diff --git a/en/constellation/octans.md b/en/constellation/octans.md index 92c708813..fa22f4547 100644 --- a/en/constellation/octans.md +++ b/en/constellation/octans.md @@ -3,7 +3,7 @@ name: Octans created_by: skybber created_date: 2021-07-10 14:40:35.924163 updated_by: skybber -updated_date: 2021-07-10 14:40:35.924395 +updated_date: 2022-12-31 17:22:52.126079 --- -![<]($IMG_DIR/cons/Oct.png) -A faint constellation in the southern sky, invisible to us, in which the south celestial pole lies. The Octant corresponds in position to the Little Chariot of the northern sky, but does not fulfill the role of Polaris, not having a star near the pole bright enough for orientation. The closest star to the south pole visible to the naked eye is Sigma Octantis, which has an apparent brightness of only 5.48mag. Octantis is a very star-poor region and of little interest to observers because it contains no bright deep-sky objects. The constellation is worthy of attention only because it contains the south celestial pole. \ No newline at end of file +![<]($IMG_DIR/cons/Oct.png) +A faint constellation in the southern sky, invisible to us, in which the south celestial pole lies. The Octans corresponds in position to the Little Dipper of the northern sky, but does not fulfill the role of Polaris, not having a star near the pole bright enough for orientation. The closest star to the south pole visible to the naked eye is Sigma Octantis, which has an apparent brightness of only 5.48mag. Octantis is a very star-poor region and of little interest to observers because it contains no bright deep-sky objects. The constellation is worthy of attention only because it contains the south celestial pole. \ No newline at end of file diff --git a/en/constellation/pavo.md b/en/constellation/pavo.md index df176ab01..64e3d2470 100644 --- a/en/constellation/pavo.md +++ b/en/constellation/pavo.md @@ -3,8 +3,8 @@ name: Pavo created_by: skybber created_date: 2021-07-11 10:22:28.106270 updated_by: skybber -updated_date: 2021-07-11 10:22:28.106574 +updated_date: 2023-01-01 15:57:15.093478 --- -Not most prominently the constellation of the southern sky, between Sagittarius and the south celestial pole. Not visible here. The brightest star of the constellation α Pavona is usually referred to by the English name Peacock, which simply means "peacock". - +Not most prominently the constellation of the southern sky, between Sagittarius and the south celestial pole. Not visible here. The brightest star of the constellation α Pavona is usually referred to by the English name "Peacock". + ![<]($IMG_DIR/cons/Pav.png) \ No newline at end of file diff --git a/en/constellation/phoenix.md b/en/constellation/phoenix.md index 6478d6ff1..03f80babd 100644 --- a/en/constellation/phoenix.md +++ b/en/constellation/phoenix.md @@ -3,8 +3,8 @@ name: Phoenix created_by: skybber created_date: 2021-07-17 17:52:15.161132 updated_by: skybber -updated_date: 2021-07-17 17:52:15.161448 +updated_date: 2023-01-01 16:15:42.485215 --- -A constellation of the southern sky lying outside the Milky Way between Fomalhaut of the Southern Fish and Achernar of Eridanus. Only the northern part of the constellation rises 1 degree above the horizon during the autumn months. Just above the horizon the whole constellation appears only in the southern regions of the Mediterranean. With the exception of the star SX Phoenicia, Phoenix contains essentially no objects of interest. In this part of the sky, however, a view of the world of distant (faint) galaxies is uncovered. The quartet of NGC 87-88-89 and NGC 92, 180 million light-years away, is a tour of different types of star systems in large telescopes: NGC 87 is an irregular galaxy, NGC 88 is a spiral galaxy with an outer gas envelope, NGC 89 has two distinctive broad arms, and NGC 92 has one exceptionally long spiral arm. - -![<]($IMG_DIR/cons/Phe.png) +A constellation of the southern sky lying outside the Milky Way between Fomalhaut of the Piscis Austrinus and Achernar of Eridanus. Only the northern part of the constellation rises 1 degree above the horizon during the autumn months. Just above the horizon the whole constellation appears only in the southern regions of the Mediterranean. With the exception of the star SX Phoenicia, Phoenix contains essentially no objects of interest. In this part of the sky, however, a view of the world of distant (faint) galaxies is uncovered. The quartet of NGC 87-88-89 and NGC 92, 180 million light-years away, is a tour of different types of star systems in large telescopes: NGC 87 is an irregular galaxy, NGC 88 is a spiral galaxy with an outer gas envelope, NGC 89 has two distinctive broad arms, and NGC 92 has one exceptionally long spiral arm. + +![<]($IMG_DIR/cons/Phe.png) diff --git a/en/constellation/pictor.md b/en/constellation/pictor.md index 2767b1f58..c8dac5006 100644 --- a/en/constellation/pictor.md +++ b/en/constellation/pictor.md @@ -3,8 +3,8 @@ name: Pictor created_by: skybber created_date: 2021-07-17 17:53:14.155703 updated_by: skybber -updated_date: 2021-07-17 17:53:14.155996 +updated_date: 2023-01-02 17:50:43.027758 --- -A smaller and less prominent constellation in the southern sky, not visible here. This monotonous group of stars lies below the dove, just west of the very bright star Canopus in the constellation of the keel. The most famous object in this small southern constellation is Kapteyn's Star, the red dwarf closest to Earth and space. A source of radiation that can be observed at a frequency of 18.3 MHz. In 1925, an unusual nova appeared in the constellation of Painter. At the time of its discovery, it was 2nd magnitude, but gradually brightened to 1st magnitude. It then gradually faded, only to brighten again two months after its first maximum. - -![<]($IMG_DIR/cons/Pic.png) +A smaller and less prominent constellation in the southern sky, not visible here. This monotonous group of stars lies below the dove, just west of the very bright star Canopus in the constellation of the Carina. The most famous object in this small southern constellation is Kapteyn's Star, the red dwarf closest to Earth and space. A source of radiation that can be observed at a frequency of 18.3 MHz. In 1925, an unusual nova appeared in the constellation of Pictor. At the time of its discovery, it was 2nd magnitude, but gradually brightened to 1st magnitude. It then gradually faded, only to brighten again two months after its first maximum. + +![<]($IMG_DIR/cons/Pic.png) diff --git a/en/constellation/pyxis.md b/en/constellation/pyxis.md index 20ba7bf50..f19d7cc7c 100644 --- a/en/constellation/pyxis.md +++ b/en/constellation/pyxis.md @@ -3,8 +3,8 @@ name: Pyxis created_by: skybber created_date: 2021-07-17 18:04:40.391224 updated_by: skybber -updated_date: 2021-07-17 18:04:40.391537 +updated_date: 2023-01-03 17:02:29.368237 --- -A small and faint constellation of the southern sky, situated about 35 degrees below the head of Hydra, between the Bulge and the Ship's Back. The brightest stars of the constellation Compass α (3.68mag), β (3.97mag) and γ Pyxidis (4.01mag) lie almost in a straight line. The constellation is poor for observers with a binocular or small telescope, but there are a few fainter open clusters, galaxies and planetary nebulae. - +A small and faint constellation of the southern sky, situated about 35 degrees below the head of Hydra, between the Antila and the Puppis. The brightest stars of the constellation Pyxis α (3.68mag), β (3.97mag) and γ Pyxidis (4.01mag) lie almost in a straight line. The constellation is poor for observers with a binocular or small telescope, but there are a few fainter open clusters, galaxies and planetary nebulae. + ![<]($IMG_DIR/cons/Pyx.png) \ No newline at end of file diff --git a/en/constellation/reticulum.md b/en/constellation/reticulum.md index 27bd8fe2e..a7fcf4d26 100644 --- a/en/constellation/reticulum.md +++ b/en/constellation/reticulum.md @@ -3,8 +3,8 @@ name: Reticulum created_by: skybber created_date: 2021-07-19 17:55:02.112427 updated_by: skybber -updated_date: 2022-02-11 18:38:22.814719 +updated_date: 2023-01-03 17:09:49.706246 --- -A small, relatively prominent constellation in the southern sky, but not observable in our latitudes. The bright stars form a diamond pattern between Dove and Swordfish, close to the Great Magellanic Cloud, halfway between the bright stars Achernar and Canopus. All the brighter stars of the constellation, except α reticulata, which is yellow, are orange in colour, giving this small constellation a rather striking appearance in the binocular. Otherwise, there are no interesting deep-sky objects. - -![<]($IMG_DIR/cons/Ret.png) +A small, relatively prominent constellation in the southern sky, but not observable in our latitudes. The bright stars form a diamond pattern between Columba and Dorado, close to the Great Magellanic Cloud, halfway between the bright stars Achernar and Canopus. All the brighter stars of the constellation, except α Reticulata, which is yellow, are orange in colour, giving this small constellation a rather striking appearance in the binocular. Otherwise, there are no interesting deep-sky objects. + +![<]($IMG_DIR/cons/Ret.png) diff --git a/en/constellation/telescopium.md b/en/constellation/telescopium.md index b4e9045ad..ddb8b07a0 100644 --- a/en/constellation/telescopium.md +++ b/en/constellation/telescopium.md @@ -3,8 +3,8 @@ name: Telescopium created_by: skybber created_date: 2021-07-25 09:01:01.713942 updated_by: skybber -updated_date: 2021-07-25 09:01:01.714291 +updated_date: 2023-01-03 17:15:48.131979 --- -A faint and small constellation of the southern sky, which is always hidden below the horizon in our latitudes. It lies to the south of Scorpio, Sagittarius and the Southern Crown, so it understandably does not stand out much in the sky. In the constellation we find a few faint galaxies, a globular cluster and a small planetary nebula. Curiously, the constellation today lacks γ Telescopii, which has become G Scorpii in spiky Scorpius, so that the current version of the celestial telescope is considerably shorter than N. L. Lacaille's idea. - +A faint and small constellation of the southern sky, which is always hidden below the horizon in our latitudes. It lies to the south of Scorpio, Sagittarius and the Corona australis, so it understandably does not stand out much in the sky. In the constellation we find a few faint galaxies, a globular cluster and a small planetary nebula. Curiously, the constellation today lacks γ Telescopii, which has become G Scorpii in cusp of Scorpius, so that the current version of the celestial telescope is considerably shorter than N. L. Lacaille's idea. + ![<]($IMG_DIR/cons/Tel.png) \ No newline at end of file diff --git a/en/constellation/tucana.md b/en/constellation/tucana.md index 9522a9f84..a0b536a24 100644 --- a/en/constellation/tucana.md +++ b/en/constellation/tucana.md @@ -3,8 +3,8 @@ name: Tucana created_by: skybber created_date: 2021-08-01 07:36:46.181594 updated_by: skybber -updated_date: 2021-08-01 07:36:46.181827 +updated_date: 2023-01-03 17:24:11.390233 --- -A constellation near the south pole of the sky, whose brighter stars form an irregular polygon, clearly looming against the almost starless background between Crane and the Water Serpent, by the bright star Achernar of Eridania. In the Toucan is the Small Magellanic Clouds, a small irregular galaxy, a companion to our own. The second important object is the globular cluster 47 Tucanae, the most beautiful in the sky according to the subjective feelings of observers. - -![<]($IMG_DIR/cons/Tuc.png) +A constellation near the south pole of the sky, whose brighter stars form an irregular polygon, clearly looming against the almost starless background between Grus and the Hydrus, by the bright star Achernar of Eridanus. In the Tucana is the Small Magellanic Clouds, a small irregular galaxy, a companion to our own. The second important object is the globular cluster 47 Tucanae, the most beautiful in the sky according to the subjective feelings of observers. + +![<]($IMG_DIR/cons/Tuc.png) diff --git a/en/star/38_Psc.md b/en/star/38_Psc.md deleted file mode 100644 index 377e68819..000000000 --- a/en/star/38_Psc.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: 38 Psc -constellation: Psc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.374596 ---- diff --git a/en/star/Barnard's_Star.md b/en/star/Barnard's_Star.md deleted file mode 100644 index 60e577de4..000000000 --- a/en/star/Barnard's_Star.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Barnard's Star -constellation: Oph -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:58:40.395982 ---- -This interesting red star, visible only through binoculars, moves the fastest of all against the background of more distant stars - it moves 10.31" across the sky per year, or the diameter of the Moon in 180 years. It is therefore sometimes referred to as Barnard's Arrow. It has the largest proper motion of any known star, discovered by E. Barnard in 1916, and is the second closest star to our Sun after the α Centauri system, separated from it by only 5.9ly, which is also the main reason for its rapid movement across the sky. Barnard's Arrow is still getting closer to us, in the year 9700, when it will be in the head of Draco, it will be only 3.8 light years away! Recording its movements could be a very interesting activity. By plotting its position in the star field at high magnification at least once a year, we can see for ourselves. \ No newline at end of file diff --git a/en/star/Brisbane_14.md b/en/star/Brisbane_14.md deleted file mode 100644 index d63b5e663..000000000 --- a/en/star/Brisbane_14.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Brisbane 14 -constellation: CrA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:45:36.948178 ---- -a double star observed only 12' WNW of the reflection nebula NGC 6726 -27, as an almost equally bright pair of blue-white 6.6mag and 6.8mag components that even a small telescope can resolve. The mutual distance of the components is 12.7". \ No newline at end of file diff --git a/en/star/Burnham_441.md b/en/star/Burnham_441.md deleted file mode 100644 index 7ae8c14b8..000000000 --- a/en/star/Burnham_441.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Burnham 441 -constellation: Vul -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:47:54.870937 ---- -a 100 mm telescope might have been enough to see this double star. It presents itself as a colour contrast of gold and blue components. The difference in magnitude is large, with the gold component reaching 6.2mag, the blue only 10.7mag. It lies at a distance of 5.9". \ No newline at end of file diff --git a/en/star/Burnham_800.md b/en/star/Burnham_800.md deleted file mode 100644 index 40ee8031e..000000000 --- a/en/star/Burnham_800.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Burnham 800 -constellation: Com -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:42:33.516148 ---- -a beautiful double star, despite the unequal brightness of the orange 6.6mag and the red component 9.7mag at a distance of 6.8". There is a 10.4mag star 92.5" north of the main star. We need a good quality telescope of at least 10 cm. \ No newline at end of file diff --git a/en/star/CAS_A.md b/en/star/CAS_A.md deleted file mode 100644 index 64e2c5c7d..000000000 --- a/en/star/CAS_A.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: CAS A -constellation: Cas -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:14:32.931056 ---- -the remnant of a supernova that probably appeared in the sky tens of thousands of years ago, so there is no proven record of it. Today we are imaging the strongest stellar radio source in the entire sky from this region, south of M52. At the site of the radio object, we can find filamentary nebulae expanding at 900 km/s, with a distance estimated at 10,000 light-years. \ No newline at end of file diff --git a/en/star/Cygnus_X-1.md b/en/star/Cygnus_X-1.md deleted file mode 100644 index b5213a064..000000000 --- a/en/star/Cygnus_X-1.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Cygnus X-1 -constellation: Cyg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:54:42.177288 ---- -a binary near η Cygni. It is a variable X-ray source. One component is visible, the other is invisible, but X-rays are emitted from its vicinity. The visible star is a luminous supergiant, the invisible component is probably a collapsed old star with a large mass - a black hole with a radius of only 10 km, which is siphoning off huge amounts of gas from the luminous supergiant (radius 10 million km) and emitting extremely intense X-rays before it reaches its boundary. \ No newline at end of file diff --git a/en/star/Dunlop_236.md b/en/star/Dunlop_236.md deleted file mode 100644 index d51a2a934..000000000 --- a/en/star/Dunlop_236.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Dunlop 236 -constellation: Mic -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.600630 ---- diff --git a/en/star/False_Cross.md b/en/star/False_Cross.md deleted file mode 100644 index 7e4dab8f4..000000000 --- a/en/star/False_Cross.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: False Cross -constellation: Car -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:02:33.404839 ---- -čtveřice hvězd ι, ε Car a δ a κ Velorum tvoří na obloze písmeno X, které se často zaměňuje s hvězdami Jižního kříže. Falešný kříž je ale o něco větší, symetričtější a méně jasný. ε Car je pěknou dvojhvězdou rozlišitelný v menším dalekohledu. Tvoří ji dvě složky jasnosti 3mag a 6mag, od sebe vzdáleny 5 ". \ No newline at end of file diff --git a/en/star/Groombridge_1830.md b/en/star/Groombridge_1830.md deleted file mode 100644 index 40954a902..000000000 --- a/en/star/Groombridge_1830.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Groombridge 1830 -constellation: UMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-03 20:47:00.792738 ---- -a nearby star that has the third fastest known motion after Barnard's and Kapteyn's stars - 7.04" per year. In about 100,000 years, the star will move from the Big Dipper to the constellation of the Wolf! Because it is 28 light-years away, its fast apparent motion is due to its true cosmic speed rather than its proximity. Such stars are part of the Milky Way galaxy, which is why they are as old as globular clusters. Arcturus of Shepherd is the clearest example of them. \ No newline at end of file diff --git a/en/star/Groombridge_34_(Grb_34).md b/en/star/Groombridge_34_(Grb_34).md deleted file mode 100644 index 5d7756131..000000000 --- a/en/star/Groombridge_34_(Grb_34).md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Groombridge 34 (Grb 34) -constellation: And -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:08:56.936555 ---- -a nearby red dwarf star, only 11.56 light years away, and at 8.2 mag visible even to a trier, about a quarter of a degree from 26 And. A guide of 10.6mag brightness at a distance of 35.5" will orbit it in 2,600 years. The pair has a rapid proper motion, 2.89" per year. Careful drawings made at high magnifications once a year will reveal this motion relative to the surrounding stellar field. \ No newline at end of file diff --git a/en/star/Herschel_3750.md b/en/star/Herschel_3750.md deleted file mode 100644 index 70641ca43..000000000 --- a/en/star/Herschel_3750.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Herschel 3750 -constellation: Lep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:50:33.198101 ---- -This tight yellow-white-blue double star was named by William Herschel as "the most beautiful double star". It can be easily verified with a smaller telescope. The components reach a brightness of 4.7mag and 8.4mag, and lie 4.2" apart. \ No newline at end of file diff --git a/en/star/Herschel_3780.md b/en/star/Herschel_3780.md deleted file mode 100644 index 995d960d3..000000000 --- a/en/star/Herschel_3780.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Herschel 3780 -constellation: Lep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:48:40.323623 ---- -a small cluster (NGC 2017), whose main members are listed in the Herschel catalogue. The small telescope reveals a 6mag star with four companions of 8mag to 10mag. In a larger telescope, two of the components can be verified to be close binaries. The fainter 12mag star that completes the group also appears. \ No newline at end of file diff --git a/en/star/Herschel_3857.md b/en/star/Herschel_3857.md deleted file mode 100644 index f22c94d50..000000000 --- a/en/star/Herschel_3857.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Herschel 3857 -constellation: Col -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:38:31.051250 ---- -a triple star, which in a telescope with a 100 mm objective diameter we can see as a nice wide yellow-orange pair of stars, brightness 5.7mag and 6.9mag respectively. The brighter component has a fainter gray-white guide of 10.8mag at a distance of 12.9". \ No newline at end of file diff --git a/en/star/Herschel_4423.md b/en/star/Herschel_4423.md deleted file mode 100644 index 38d3932b6..000000000 --- a/en/star/Herschel_4423.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Herschel 4423 -constellation: Cen -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:26:28.807602 ---- -an attractive pair of yellow stars dominating a rather sparse star field. The components are bright 6.9mag and 7.2mag and are spaced 2.4" apart. \ No newline at end of file diff --git a/en/star/Herschel_4788.md b/en/star/Herschel_4788.md deleted file mode 100644 index 9dc05ea72..000000000 --- a/en/star/Herschel_4788.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Herschel 4788 -constellation: Lup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:57:51.588207 ---- -a double star that is a good test for a 100-150 mm telescope. On a calm night, this unevenly bright pair of white and yellow stars appears as two disks in contact. However, if there is any turbulence in the atmosphere, the stars merge into one elongated blob. They lie 2.2" apart and their luminosities are 4.7mag and 6.7mag respectively. \ No newline at end of file diff --git a/en/star/Herschel_5003.md b/en/star/Herschel_5003.md deleted file mode 100644 index d83952cf3..000000000 --- a/en/star/Herschel_5003.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Herschel 5003 -constellation: Sgr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:40:24.238580 ---- -a triple star consisting of two red-orange stars, the brighter 5.2mag being the redder. The fainter 6.9mag star is 5.5" away. Another but very faint 13mag guide is found at a distance of 26.2" and can be resolved during a good night. These triple stars lie in a nice field of the Milky Way. \ No newline at end of file diff --git a/en/star/Herschel_84.md b/en/star/Herschel_84.md deleted file mode 100644 index e89153bb9..000000000 --- a/en/star/Herschel_84.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Herschel 84 -constellation: Sge -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:32:04.889928 ---- -a binary star consisting of a main orange (6.5mag) and a minor blue component (8.9mag) at a distance of 28.2". In at least a 100mm telescope and higher magnification, probably the most beautiful binary in the constellation. \ No newline at end of file diff --git a/en/star/Hind's_Crimson_Star_(R_Lep).md b/en/star/Hind's_Crimson_Star_(R_Lep).md deleted file mode 100644 index 4bfcd01db..000000000 --- a/en/star/Hind's_Crimson_Star_(R_Lep).md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Hind's Crimson Star (R Lep) -constellation: Lep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:50:07.807799 ---- - Like Mira Ceti, it is a red giant that changes its brightness typically between 6mag and 11.7mag over a 430-day period. The total difference between maximum and minimum corresponds to a difference in brightness of 300 times. There is also a long secondary cycle - every 40 years the star brightens to 5.5mag. At its brightest, it resembles a deep red drop of blood in a dark sky and is visible to the naked eye. It is located near μ Lep (3.31mag). R Leporel is a giant star with a low surface temperature of about 2,700 K, with carbon molecules in its atmosphere that absorb shortwave radiation and a large dust cloud surrounding it. All of this accounts for the star's red colour, which stands out especially at times of maximum brightness. The star is visible to the trier, but binoculars are needed to see the colour clearly. \ No newline at end of file diff --git a/en/star/Kapteynova_hviezda.md b/en/star/Kapteynova_hviezda.md deleted file mode 100644 index 944d51ddb..000000000 --- a/en/star/Kapteynova_hviezda.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Kapteynova hviezda -constellation: Pic -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.396121 ---- diff --git a/en/star/Keplerova_supernova.md b/en/star/Keplerova_supernova.md deleted file mode 100644 index d631e8f5c..000000000 --- a/en/star/Keplerova_supernova.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Keplerova supernova -constellation: Oph -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:57:44.864694 ---- -the last galactic supernova, which exploded on September 9, 1604. It is named after a famous German astronomer who observed it in those days. It was visible to the naked eye for 12 months, and for several weeks its brightness of -2.5 mag surpassed even the planet Jupiter. Johannes Kepler and David Fabricius pinpointed its position with such accuracy that the German-born American astronomer Walter Baade was able to identify a faint nebula, a supernova remnant, in the same place in 1943. The star itself is now fainter than 19mag and can only be observed with the largest telescopes. The Hubble Space Telescope has detected its remnant. \ No newline at end of file diff --git a/en/star/Kruger_60.md b/en/star/Kruger_60.md deleted file mode 100644 index 7aeebe5e1..000000000 --- a/en/star/Kruger_60.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Kruger 60 -constellation: Cep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 13:42:38.399054 ---- -though invisible to the naked eye, otherwise a well-known and interesting binary star. It lies 43' south of δ Cephei. A minimum of 120mm binoculars and high magnification will be needed to resolve the main component of 9.8mag brightness and its companion 11.3mag, as they lie 2.4 arc seconds apart. It is located at a distance of only 13.1 light years, making it one of our closest binaries. The mutual orbit of these red dwarfs is only 44.5 years. Their mean distance is 1.4 billion km, which is equivalent to the Sun-Saturn distance. The mass of the main star is about 0.25 of the mass of the Sun, and the mass of its companion is only 0.15 of the mass of the Sun, and their luminosities are even smaller. \ No newline at end of file diff --git a/en/star/Lacaille_9352.md b/en/star/Lacaille_9352.md deleted file mode 100644 index 3fbb49fa2..000000000 --- a/en/star/Lacaille_9352.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Lacaille 9352 -constellation: PsA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:26:29.751258 ---- -a red dwarf of visual magnitude 7.4. It shows the fourth fastest known proper motion after Barnard's and Kapteyn's stars and the Great Bear star Groombridge 1830, Lacaille 9352. In one year, this star will have moved 6.9", and by 2100 it will be in the neighboring constellation of Sculptor. It lies at a distance of just 10.7 ly. \ No newline at end of file diff --git a/en/star/Lalande_21185.md b/en/star/Lalande_21185.md deleted file mode 100644 index 6870c24d9..000000000 --- a/en/star/Lalande_21185.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Lalande 21185 -constellation: UMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-03 20:47:24.667929 ---- -a nearby red dwarf that reaches a brightness of 7.49mag. It lies at a distance of 8.1 light-years and is our fourth closest star after Alpha Centauri, Barnard's Star of Hadonos and Wolf 359 of Leo. It has the 8th largest known proper motion - it moves 4.78" across the sky each year. This red dwarf has an absolute magnitude of +10.5, equivalent to 0.0048 the luminosity of the Sun. Lalande 21185 has a companion, but it has never been visually observed. \ No newline at end of file diff --git a/en/star/Musca_Borealis.md b/en/star/Musca_Borealis.md deleted file mode 100644 index 31a64138e..000000000 --- a/en/star/Musca_Borealis.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Musca Borealis -constellation: Ari -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:32:43.906730 ---- -a now-defunct constellation that once consisted of the three stars of the constellation Aries - 35, 39, 41 Arietis, representing the buzzing flies of the sea perched on Aries' tail. \ No newline at end of file diff --git a/en/star/N_1918_Aql.md b/en/star/N_1918_Aql.md deleted file mode 100644 index f64a4358c..000000000 --- a/en/star/N_1918_Aql.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: N 1918 Aql -constellation: Aql -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:26:14.053778 ---- -After Nova, which appeared in Eagle in 389 and became brighter than Venus, astronomers were treated to another in 1918. It became the brightest star in the constellation and the second brightest star in the sky after the spread, reaching -1.1mag. Today it is not visible to the naked eye, not even a trier, reaching only 10.8mag. \ No newline at end of file diff --git a/en/star/N_1991.md b/en/star/N_1991.md deleted file mode 100644 index 1efd48c3f..000000000 --- a/en/star/N_1991.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: N 1991 -constellation: Mus -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.373348 ---- diff --git a/en/star/N_Hya.md b/en/star/N_Hya.md deleted file mode 100644 index fd184046d..000000000 --- a/en/star/N_Hya.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: N Hya -constellation: Hya -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:44:55.396720 ---- -a nice almost equally bright pair of yellow 5.8mag, 5.9mag components, easily distinguishable in small telescopes, the components lie at a distance of 9.2". In the same field of view we can further see a single red-orange star, 8' to the northeast. \ No newline at end of file diff --git a/en/star/Nova_Delphini_1967.md b/en/star/Nova_Delphini_1967.md deleted file mode 100644 index fcf6f1b14..000000000 --- a/en/star/Nova_Delphini_1967.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Nova Delphini 1967 -constellation: Del -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:58:48.628007 ---- -the constellation was made famous by the nova discovered on July 8, 1967 by the English teacher, amateur astronomer G. Alcock, who, among other things, discovered the nova Vulpeculae 1968. The strange nova slowly brightened n2several thousand times and became visible even to the naked eye, then its brightness fluctuated irregularly, and in December 1967 it dimmed again . According to records, it is "the slowest nova". Its current magnitude is approximately 12.7mag, making it visible only with a slightly larger amateur telescope. \ No newline at end of file diff --git a/en/star/P_Hya.md b/en/star/P_Hya.md deleted file mode 100644 index 2382605cf..000000000 --- a/en/star/P_Hya.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: P Hya -constellation: Hya -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:44:35.449849 ---- -easily distinguishable 5mag and 6.9mag components at 4' separation. Through a 60mm diameter telescope, we find that the fainter component has a 9th magnitude guide at a distance of 9.6". \ No newline at end of file diff --git a/en/star/Plaskett_star.md b/en/star/Plaskett_star.md deleted file mode 100644 index 85882f154..000000000 --- a/en/star/Plaskett_star.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Plaskett star -constellation: Mon -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 10:13:55.332535 ---- -a spectral binary star of sixth magnitude discovered in 1922 by Canadian astronomer and director of the Victoria Observatory John Stanley Plaskett. It is the most massive binary star known. \ No newline at end of file diff --git a/en/star/Proxima_Centauri.md b/en/star/Proxima_Centauri.md deleted file mode 100644 index 615b1d88c..000000000 --- a/en/star/Proxima_Centauri.md +++ /dev/null @@ -1,11 +0,0 @@ ---- -name: Proxima Centauri -constellation: Cen -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:24:42.633336 ---- -![]($IMG_DIR/dso/Proxima.jpg) - -In 1915, R. T. Innes measured the proper motions of stars around α Centauri. At a distance of 2.2 arc degrees southwest of this star, he found a star of brightness 10.7mag moving in the same direction and speed as both components of α Centauri. This red dwarf is actually our closest star to the Sun, only 4.25 light-years away. It probably belongs to the α Centauri system, even though it orbits it at a very great distance. Yet in a few thousand years, when it gets past Toliman, it will no longer be our nearest star. Proxima - which means "nearest" in Latin - will occasionally brighten by more than half a magnitude and usually return to its original brightness in half an hour. Proxima Centauri is a small star, with a mass of only 1/10 that of the Sun, and is very faint, shining less than 0.0008 of the Sun. \ No newline at end of file diff --git a/en/star/RR_Lyrae.md b/en/star/RR_Lyrae.md deleted file mode 100644 index d05031562..000000000 --- a/en/star/RR_Lyrae.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: RR Lyrae -constellation: Lyr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:52:11.152132 ---- -this star, lying on the border with the Cygnus, invisible to the naked eye, is a representative of an important class of variable stars whose brightness varies in a short period. They are old stars found mainly around the Galactic centre and in globular clusters, the oldest formations in the galaxy. RR Lyra pulses periodically, like Delta Cephei, but its period is less than a day - 0.567 days. In that time - 13 hours and 36 minutes - the apparent brightness varies from 7mag to 8.1mag. The cycle can therefore be observed (from some areas) in virtually one night. At its maximum it is white, at its minimum it takes on a yellowish tint. \ No newline at end of file diff --git a/en/star/RR_Tel.md b/en/star/RR_Tel.md deleted file mode 100644 index 218685046..000000000 --- a/en/star/RR_Tel.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: RR Tel -constellation: Tel -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 10:53:13.639083 ---- -Although this star is too faint for a small telescope, it is one of the most interesting novae recorded in our history. Before 1945, its brightness for 13 months fluctuated between 12.5mag and 15mag. But then it burst into flames and held its brightness at magnitude 6.5 for 5 years. Although it later faded to its original brightness, it still retained its original period of brightness changes. It is definitely a binary star, the larger component of which is a red giant changing brightness, while the smaller component is a hot dense star that flared as a nova. \ No newline at end of file diff --git a/en/star/RS_Oph.md b/en/star/RS_Oph.md deleted file mode 100644 index 6dbeb352b..000000000 --- a/en/star/RS_Oph.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: RS Oph -constellation: Oph -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:56:54.319363 ---- -a recurrent nova that flared up successively in 1898, 1933, 1958, 1967 and 1985. At minimum it has a brightness of 11.8mag, and at outburst sometimes as high as 4.3mag. \ No newline at end of file diff --git a/en/star/RW_Tauri.md b/en/star/RW_Tauri.md deleted file mode 100644 index efeff5877..000000000 --- a/en/star/RW_Tauri.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: RW Tauri -constellation: Tau -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 09:56:49.265873 ---- -occulting variable star, one degree northwest of 41 Tauri. The main component is completely occulted for good every 2.76 days, which diminishes its brightness from 7.9mag to 11.4mag. The total occultation lasts 9 hours, with the entire eclipse lasting 84 minutes. Among eclipsing variable stars, RW Tauri shows one of the deepest magnitude declines, by as much as 3.5. The system is estimated to be 1 370 light years away. diff --git a/en/star/RX_J185635-3754.md b/en/star/RX_J185635-3754.md deleted file mode 100644 index 7c1c1ff7f..000000000 --- a/en/star/RX_J185635-3754.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: RX J185635-3754 -constellation: CrA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:46:37.327137 ---- -under this obscure designation is our nearest neutron star, which lies 200 light-years away. With its apparent brightness of 26mag, it can't be observed in any way, and was only discovered in 1996 by the Hubble Space Telescope. It's the remnant of a supernova explosion a million years ago. \ No newline at end of file diff --git a/en/star/R_Ara.md b/en/star/R_Ara.md deleted file mode 100644 index 59487bdfc..000000000 --- a/en/star/R_Ara.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Ara -constellation: Ara -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:29:06.033615 ---- -an eclipsing variable star of the Algol type, with a period of 4.4 days and a magnitude variation from 6.0 to 6.9. It is in the field of view of the binocular along with the stars ζ and η Ara. \ No newline at end of file diff --git a/en/star/R_Cae.md b/en/star/R_Cae.md deleted file mode 100644 index 9cfc9cdab..000000000 --- a/en/star/R_Cae.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Cae -constellation: Cae -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 18:20:41.422440 ---- -a relatively bright variable star of the Mira Ceti type that varies its brightness between 6.7mag and 13.7mag over a period of more than 13 months. \ No newline at end of file diff --git a/en/star/R_Casiopeiae.md b/en/star/R_Casiopeiae.md deleted file mode 100644 index 8d49c5616..000000000 --- a/en/star/R_Casiopeiae.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Casiopeiae -constellation: Cas -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:16:08.448017 ---- -A long-period variable star with a magnitude range from 4.7 to 13.5 over 431 days. It is located closer to the boundary with the constellation Andromeda. \ No newline at end of file diff --git a/en/star/R_Com.md b/en/star/R_Com.md deleted file mode 100644 index fe1d95782..000000000 --- a/en/star/R_Com.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Com -constellation: Com -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:41:55.201581 ---- -a variable star of the type Mira Ceti with magnitude variations from 7.1 to 14.6 over a period of 363 days. \ No newline at end of file diff --git a/en/star/R_Corvi.md b/en/star/R_Corvi.md deleted file mode 100644 index 568274d8d..000000000 --- a/en/star/R_Corvi.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Corvi -constellation: Crv -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 17:05:04.827986 ---- -The orange-red Mira-type variable star varies its brightness from magnitude 6.7 to 14.4 over a period of 10 months to 317 days. It forms the western apex of a triangle with two 7.5-mag stars. At its maximum it shines through, while at its minimum it is barely visible even in a larger telescope. \ No newline at end of file diff --git a/en/star/R_Hydrae.md b/en/star/R_Hydrae.md deleted file mode 100644 index d3b366856..000000000 --- a/en/star/R_Hydrae.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Hydrae -constellation: Hya -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:44:10.602134 ---- -a red giant, one of the most famous Mira Ceti type variable stars. It varies in apparent brightness from 3.5mag to 10.9mag over a period of 389.6 days, first noticed by astronomers in the 17th century. However, the period has probably shortened by about 100 days since then. It is about 700 light-years away and at its greatest peak exceeds the luminosity of 7,000 Suns. \ No newline at end of file diff --git a/en/star/R_LMi.md b/en/star/R_LMi.md deleted file mode 100644 index d57a715e1..000000000 --- a/en/star/R_LMi.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R LMi -constellation: LMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:44:16.394014 ---- -Mira-type variable star, similar in many ways to the red supergiant R Leonis. It has a period of about 372 days and varies in brightness from 6.3mag to 13.2mag, thus disappearing from the range of small telescopes. It lies 45' southeast of the star 13 LMI, which has a brightness of 6.2mag. \ No newline at end of file diff --git a/en/star/R_Oct.md b/en/star/R_Oct.md deleted file mode 100644 index 995173eb7..000000000 --- a/en/star/R_Oct.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: R Oct -constellation: Oct -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.868079 ---- diff --git a/en/star/R_Ret.md b/en/star/R_Ret.md deleted file mode 100644 index 60ce874d5..000000000 --- a/en/star/R_Ret.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Ret -constellation: Ret -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-08 14:48:17.369418 ---- -a red Mira-type star reaching 7mag at its maximum. It will return to its minimum brightness of 13mag after about 9 months. \ No newline at end of file diff --git a/en/star/R_TrA.md b/en/star/R_TrA.md deleted file mode 100644 index 1cbbb0abf..000000000 --- a/en/star/R_TrA.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R TrA -constellation: TrA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-03 08:10:35.759862 ---- -Cepheid changing its brightness by less than one magnitude: 6-6.8mag in a period of 3.389 days. For such a rapidly changing Cepheids, determining its brightness once a night is insufficient. \ No newline at end of file diff --git a/en/star/R_a_S_Gru.md b/en/star/R_a_S_Gru.md deleted file mode 100644 index 8ebd4c66d..000000000 --- a/en/star/R_a_S_Gru.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: R a S Gru -constellation: Gru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.205572 ---- diff --git a/en/star/R_a_TW_Hor.md b/en/star/R_a_TW_Hor.md deleted file mode 100644 index bb0ac14c3..000000000 --- a/en/star/R_a_TW_Hor.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: R a TW Hor -constellation: Hor -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.058648 ---- diff --git a/en/star/SN1987A.md b/en/star/SN1987A.md deleted file mode 100644 index f1ce4f1b1..000000000 --- a/en/star/SN1987A.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: SN1987A -constellation: Dor -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:15:51.376551 ---- -a bright supernova that shone in the Large Magellanic Cloud in the vicinity of the Tarantula Nebula on 23 February 1987, reaching its maximum of 2.8 mag. Thus, after 383 years since Kepler's supernova, at least residents of the southern hemisphere could marvel at another supernova visible to the naked eye. It shone in the sky for 10 months, but is now very faint. It probably left behind a pulsar that has not yet been found. \ No newline at end of file diff --git a/en/star/SN_1006.md b/en/star/SN_1006.md deleted file mode 100644 index bee2ca4a7..000000000 --- a/en/star/SN_1006.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: SN 1006 -constellation: Lup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:56:39.704566 ---- -the brightest supernova ever recorded in human history. It was noticed by the inhabitants of China and Japan, as well as the Middle East and Europe. When it first appeared in the sky in the spring of 1006, it was about as bright as Mars in opposition. Within a few weeks, however, it easily surpassed Venus, brightening to -7.5mag, equivalent to the brightness of the Moon in the first quarter. The supernova was visible for the next two years, even briefly during the day. Today, all we see at this site is a cloud of debris from the ancient stellar explosion. \ No newline at end of file diff --git a/en/star/SS_Cygni.md b/en/star/SS_Cygni.md deleted file mode 100644 index 1d1a1f7c7..000000000 --- a/en/star/SS_Cygni.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: SS Cygni -constellation: Cyg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:55:14.348561 ---- -one of the many variable stars is a cataclysmic variable star that flares up every 2 months to a brightness of 8mag, but is normally a 12mag star. It is the prototype of the dwarf stars known as either SS Cygni or U Geminorum type variable stars. \ No newline at end of file diff --git a/en/star/SX_Phe.md b/en/star/SX_Phe.md deleted file mode 100644 index c8f2074bf..000000000 --- a/en/star/SX_Phe.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: SX Phe -constellation: Phe -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.767543 ---- diff --git a/en/star/S_Aps.md b/en/star/S_Aps.md deleted file mode 100644 index b15fca879..000000000 --- a/en/star/S_Aps.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: S Aps -constellation: Aps -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:14:05.751220 ---- -this star is the new "opposite". It's usually brighter than 10mag, so even a small telescope can pick it up, but it seems to be blowing dark material irregularly into its surroundings, reducing its brightness 100 times to 15mag. After a few weeks, when its veil has dissipated into its surroundings, it will shine back to its original brilliance. \ No newline at end of file diff --git a/en/star/S_Doradus.md b/en/star/S_Doradus.md deleted file mode 100644 index 0e706861c..000000000 --- a/en/star/S_Doradus.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: S Doradus -constellation: Dor -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:16:22.631677 ---- -an exceptionally luminous star that surpasses the Sun by at least a million times in luminosity. It is one of the brightest stars ever. However, because of its distance, we cannot see it with the naked eye, and we only perceive it as a faint star whose brightness varies between 8mag and 11.5mag because it is an eclipsing variable star. Its components are between 1 400 and 1 200 times the diameter of our Sun. Its absolute brightness is about -11. \ No newline at end of file diff --git a/en/star/S_Vol.md b/en/star/S_Vol.md deleted file mode 100644 index 19b09415f..000000000 --- a/en/star/S_Vol.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: S Vol -constellation: Vol -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-24 07:39:51.838960 ---- -a Mira-type variable star whose maximum is usually around 8.6mag, sometimes even 7.7mag. However, it only dips to 13.6mag at its minimum. This whole cycle takes place over a period of 14 months. \ No newline at end of file diff --git a/en/star/S_a_U_Oct.md b/en/star/S_a_U_Oct.md deleted file mode 100644 index a90c55006..000000000 --- a/en/star/S_a_U_Oct.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: S a U Oct -constellation: Oct -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.457214 ---- diff --git a/en/star/Struve_1095.md b/en/star/Struve_1095.md deleted file mode 100644 index 5d401c8b9..000000000 --- a/en/star/Struve_1095.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 1095 -constellation: CMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:55:10.504378 ---- -a double star for smaller telescopes, two stars of 8.4mag and 8.9mag lie in the sky at a distance of 10.1". Although relatively faint, it is easy to find as it lies 12' SW of γ CMI and 25' north of β CMI. Using 100x magnification, it is a lovely little pair of white main and blue minor components. \ No newline at end of file diff --git a/en/star/Struve_1104.md b/en/star/Struve_1104.md deleted file mode 100644 index 4eb89927e..000000000 --- a/en/star/Struve_1104.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 1104 -constellation: Pup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 12:02:25.281293 ---- -a beautiful but tight pair of golden yellow stars, but one that requires good seeing to see clearly. The 6.4mag and 7.5mag brightness components are separated by 2.1". \ No newline at end of file diff --git a/en/star/Struve_1149.md b/en/star/Struve_1149.md deleted file mode 100644 index 0822f572e..000000000 --- a/en/star/Struve_1149.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 1149 -constellation: CMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:56:19.288886 ---- -a binary observed 3 degrees southeast of Procyon, at the western end of the E-W belt of bright stars. In small telescopes it shows a nice yellow 7.6mag and a blue 9.6mag component, fainter copies of the star Eta of Cassiopeia. At higher magnifications, the guide may take on a purple hue. Offset 21.7". \ No newline at end of file diff --git a/en/star/Struve_1441.md b/en/star/Struve_1441.md deleted file mode 100644 index e7b1d5ed9..000000000 --- a/en/star/Struve_1441.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 1441 -constellation: Sex -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 12:03:57.843786 ---- -a tight, attractive pair that can be resolved with binoculars with a lens diameter of about 100mm at a distance of 2.6". The brighter orange component has a brightness of 6.4mag, the fainter blue 9.9mag. \ No newline at end of file diff --git a/en/star/Struve_1788.md b/en/star/Struve_1788.md deleted file mode 100644 index f6bd6ec52..000000000 --- a/en/star/Struve_1788.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 1788 -constellation: Vir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-04 20:33:33.415154 ---- -a four-pointed star, a close pair of two magnificent yellow stars (6.5mag and 7.7mag) at a distance of 3.4", accompanied by two other, much fainter components of 10.3 and 10.9mag. Recommendations: 100-150 mm and at least 100x magnification. \ No newline at end of file diff --git a/en/star/Struve_2303.md b/en/star/Struve_2303.md deleted file mode 100644 index 1332dae13..000000000 --- a/en/star/Struve_2303.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 2303 -constellation: Ser -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:29:15.659075 ---- -a close binary star observed in a Milky Way field of dark nebulae. The 6.6mag and 9.1mag components at 2.1" are a very good quality test for small telescopes and need at least 150x magnification. \ No newline at end of file diff --git a/en/star/Struve_2306.md b/en/star/Struve_2306.md deleted file mode 100644 index 0a9fca647..000000000 --- a/en/star/Struve_2306.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 2306 -constellation: Sct -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:45:46.159098 ---- -a triple star observed 1.75 degrees WNW of the star γ Scuti. The AB pair consists of a golden (7.9mag) and a bluish component (8.6mag) that lie 10.2" apart. The guide is also a tight pair that requires quite high magnification to resolve. \ No newline at end of file diff --git a/en/star/Struve_2373.md b/en/star/Struve_2373.md deleted file mode 100644 index 1ce8b1c8f..000000000 --- a/en/star/Struve_2373.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 2373 -constellation: Sct -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:46:03.623112 ---- -a binary star located in the Milky Way's rich star field. It is made up of two yellow components of 7.2mag and 8.2mag, which lie at a distance of 4.2" from each other. A reasonable minimum for resolution would be a telescope with a 10 cm objective lens diameter. \ No newline at end of file diff --git a/en/star/Struve_2455.md b/en/star/Struve_2455.md deleted file mode 100644 index 33927e8c9..000000000 --- a/en/star/Struve_2455.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 2455 -constellation: Vul -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:48:17.803035 ---- -a triple star, an attractive pair of one white and two bluish components in a 100 mm telescope. The brightest components (7.4mag and 8.5mag) lie at a distance of 6.6". Half a degree to the SSV, the binary Struve 2457 is in the same field of view, consisting of a white 7.5mag and a bluish 9mag component lying at a mutual distance of 10.3". \ No newline at end of file diff --git a/en/star/Struve_2470-slash-2474.md b/en/star/Struve_2470-slash-2474.md deleted file mode 100644 index 9ba9fe955..000000000 --- a/en/star/Struve_2470-slash-2474.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 2470/2474 -constellation: Lyr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:51:09.453716 ---- -another double binary in the constellation, observed northeast of γ Lyra. The two main stars lie just over 10' apart. In at least a 10 cm telescope, Struve 2470 resolves into two stars that lie 13.4" apart: a white and a light blue, the former with a brightness of 6.6mag, the latter with a brightness of 8.6mag. The bright yellow components of Struve 2474 lie at a distance of 16.2" and have brightnesses of 6.7mag and 8.8mag, respectively. \ No newline at end of file diff --git a/en/star/Struve_2540.md b/en/star/Struve_2540.md deleted file mode 100644 index 14ece1e99..000000000 --- a/en/star/Struve_2540.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 2540 -constellation: Vul -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:48:40.455418 ---- -the triple stars. In the 100/150 mm instrument, the relatively tight pair (5.1") consists of an unequally bright white 7.3mag and a bluish 8.8mag component. The 12.4mag guide lies 147" away. \ No newline at end of file diff --git a/en/star/Struve_2653.md b/en/star/Struve_2653.md deleted file mode 100644 index eee5c1b5d..000000000 --- a/en/star/Struve_2653.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 2653 -constellation: Vul -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:47:33.762023 ---- -The double star, in a telescope with a lens diameter of up to 150 mm, is a very close pair of unequally bright yellow-white stars (6.9mag, 9.7mag) that require adequate magnification for resolution. They lie only 2.6" apart. \ No newline at end of file diff --git a/en/star/Struve_2793.md b/en/star/Struve_2793.md deleted file mode 100644 index 6a6dae55d..000000000 --- a/en/star/Struve_2793.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 2793 -constellation: Equ -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:42:19.555809 ---- -an easily distinguishable double star even for small telescopes. The main component is yellow (7.8mag) and the guide is bluish (8.5mag). It lies at a distance of 26.6". The main star has another guide at a distance of only 0.4", but it does not resolve using high magnification. \ No newline at end of file diff --git a/en/star/Struve_2902.md b/en/star/Struve_2902.md deleted file mode 100644 index 2258c5e2a..000000000 --- a/en/star/Struve_2902.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 2902 -constellation: Lac -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-02 13:54:34.307650 ---- -multiple star, brighter 6.4" close pair consisting of a yellow (7.6mag) and a white component (8.5mag). The second pair lies to the northeast and consists of two components of brightness 12.1mag and 12.9mag at 5" apart. There are two other pairs in the same field of view. One at a closer spacing, the other at a wider spacing. A telescope with a 150 mm objective diameter is needed to examine the surroundings. \ No newline at end of file diff --git a/en/star/Struve_475.md b/en/star/Struve_475.md deleted file mode 100644 index 2d6fa5f07..000000000 --- a/en/star/Struve_475.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Struve 475 -constellation: Lac -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-02 13:54:59.632955 ---- -a nice unevenly bright double star (6.8mag and 10.8mag). The brighter star is white, the fainter guide lying 15.5" away is bluish. Immediately to the southwest lies a fainter pair of double components \ No newline at end of file diff --git a/en/star/Sualocin_a_Rotanev.md b/en/star/Sualocin_a_Rotanev.md deleted file mode 100644 index 5076feb48..000000000 --- a/en/star/Sualocin_a_Rotanev.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Sualocin a Rotanev -constellation: Del -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:56:59.125658 ---- -α (3.77mag) and β Del (3.63mag), the constellation's two brightest stars, exemplify the unquenchable human desire to leave something lasting behind. If we read the names of these stars backwards, we discover the words Nicolaus Venator, the Latin name of the Palermo astronomer Niccolo Cacciatore, a long-time assistant to the famous Italian astronomer Giuseppe Piazzi. He was anxious to keep his name in the sky. So he used a ruse and gave the two stars their own names, even though no one has the right to name a star after themselves. This lie was discovered too late, however, and the names have in the meantime caught on, and even today some atlases give them as names of unknown origin. They are the only stars in the sky that bear the name of a real person. \ No newline at end of file diff --git a/en/star/Sírius_B.md b/en/star/Sírius_B.md deleted file mode 100644 index 40cf0b102..000000000 --- a/en/star/Sírius_B.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Sírius B -constellation: CMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:51:28.002457 ---- -In 1834, Friedrich Bessel discovered that Sirius periodically swings out of position, which could only mean one thing: the star is accompanied by an invisible companion. However, telescopes of the time could not detect it. The big event did not come until three decades later, in 1862, when the American optician Alvan G. Clark, a brilliant telescope designer, while testing his new 460 mm refractor in close proximity to Sirius, a faint star, later called Sirius B - also called "Puppy" in Anglo-Saxon areas. It was not until 1915, however, that its true physical nature was discovered, making it the first white dwarf ever discovered. \ No newline at end of file diff --git a/en/star/T_Borealis.md b/en/star/T_Borealis.md deleted file mode 100644 index a0963cc20..000000000 --- a/en/star/T_Borealis.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: T Borealis -constellation: Boo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.146703 ---- diff --git a/en/star/T_Col.md b/en/star/T_Col.md deleted file mode 100644 index 63809dc2d..000000000 --- a/en/star/T_Col.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: T Col -constellation: Col -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:37:45.664827 ---- -a Mira-type variable star with a maximum of 6.7mag and a minimum of 12.6mag. Its period is 266 days. \ No newline at end of file diff --git a/en/star/T_Pyxidis.md b/en/star/T_Pyxidis.md deleted file mode 100644 index 7ba8aa80a..000000000 --- a/en/star/T_Pyxidis.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: T Pyxidis -constellation: Pyx -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.883508 ---- diff --git a/en/star/T_Tauri.md b/en/star/T_Tauri.md deleted file mode 100644 index 7ccdee975..000000000 --- a/en/star/T_Tauri.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: T Tauri -constellation: Tau -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 09:57:24.371752 ---- -observed 1.8 degrees west of ε Tauri, the star at the northern tip of the "V" Hyades, is a faint variable star of irregular period, with a mysterious emission/reflection nebula called the Hind Variable Nebula (NGC 1554 - 55). The brightness of the star varies unpredictably from 8.4mag to 13.5mag. T Tauri is a very young star, NGC 1555 is probably a remnant of the cloud from which it was born. T Tauri and NGC 1555 lie within the relatively close, 450-500 ly distant Taurus dark cloud complex, which contains other, much fainter similar stars. diff --git a/en/star/Trapezium.md b/en/star/Trapezium.md deleted file mode 100644 index 382eaaf2e..000000000 --- a/en/star/Trapezium.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Trapezium -constellation: Ori -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:58:25.913065 ---- -The "theta system", lies at the heart of the Great Nebula itself in Orion and is one of the most famous multiple stars in the entire sky. Its four stars, ranging in brightness from 5mag to 8mag, form a quadrangle called Trapezium. Several 11mag stars within and around the quadrangle are undoubtedly physically part of the Trapezium system. What's more, within the 5' area of Trapezium are over 400 very faint stars, extremely young objects recently born from huge clouds of gas and dust. The stars of Trapezium are extremely young, approximately 30,000 years old. \ No newline at end of file diff --git a/en/star/Tycho's_Supernova.md b/en/star/Tycho's_Supernova.md deleted file mode 100644 index 0507bd129..000000000 --- a/en/star/Tycho's_Supernova.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Tycho's Supernova -constellation: Cas -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:15:24.883309 ---- -or Supernova 1572, one of three supernovae observed and documented to have erupted in our Galaxy in the distant past. It was named after the Danish astronomer Tycho de Brahe, who observed its explosion on November 11, 1572, and the course of its brightness until it disappeared from the sky (it was also observed by Tadeáš Hájek of Hájek). At that time he did not know that the star exploded at a distance of 8,000 light years. The star shone in close proximity to the northwest of κ Cas. At its maximum, it was equal in apparent brightness to Venus, reaching a maximum brightness of -4.0mag, and could be seen even during the day. Then its brightness declined, but it could not be seen with the naked eye for 16 months. Today it is again a star of apparent brightness less than 19mag, with an expanding nebula, radio and X-ray source. \ No newline at end of file diff --git a/en/star/UV_Aur.md b/en/star/UV_Aur.md deleted file mode 100644 index 34e1b6cd4..000000000 --- a/en/star/UV_Aur.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: UV Aur -constellation: Aur -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:49:50.742357 ---- -a variable star that changes brightness between 7.4mag and 10.6mag over 394.4 days. At a distance of 3.4", the guide lies at 11.5mag. It is a beautiful example of a combination of orange and blue components. \ No newline at end of file diff --git a/en/star/U_Ara.md b/en/star/U_Ara.md deleted file mode 100644 index 9e11d36d9..000000000 --- a/en/star/U_Ara.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: U Ara -constellation: Ara -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:29:35.486491 ---- -a variable star of the Mira type, whose brightness is sufficient even for smaller telescopes - it reaches 8mag at its maximum. At minimum, however, its brightness drops by a full five magnitudes. It changes over a period of seven months. \ No newline at end of file diff --git a/en/star/U_Cep.md b/en/star/U_Cep.md deleted file mode 100644 index d6107dbc2..000000000 --- a/en/star/U_Cep.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: U Cep -constellation: Cep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 13:43:15.608721 ---- -an interesting short-period variable star. The brighter B-type component is occulted by a larger but fainter G giant once every 2.5 days. It varies in brightness from 6.7mag to 9.2mag, with a four-hour descent to minimum followed by two hours of total occultation. Because of the close actual separation, the brighter component of the dim giant strips a lot of material from the outer layer, resulting in the orbital period being reduced by 4 minutes over the past century. A nearby third component also appears to be part of the system, but it does not orbit in this orbit. \ No newline at end of file diff --git a/en/star/VW_Hyi.md b/en/star/VW_Hyi.md deleted file mode 100644 index 0cb1c20bc..000000000 --- a/en/star/VW_Hyi.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: VW Hyi -constellation: Hyi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.041673 ---- diff --git a/en/star/V_Hya.md b/en/star/V_Hya.md deleted file mode 100644 index 111b80e29..000000000 --- a/en/star/V_Hya.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: V Hya -constellation: Hya -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:45:17.219413 ---- -a rare example of a carbon star. It's a low-temperature red giant that produces carbon. The star is very red, so it can't be mistaken for any other star. But it has one catch: it changes its brightness irregularly between 6th and 12th mag in two main periods - 18 months and 18 years. \ No newline at end of file diff --git a/en/star/V_Sge.md b/en/star/V_Sge.md deleted file mode 100644 index e4874dff2..000000000 --- a/en/star/V_Sge.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: V Sge -constellation: Sge -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:32:29.986784 ---- -probably once a "new star", now almost at the limit of visibility even in the binocular. Almost every night it is differently bright, changing magnitude erratically from 8.6 to 13.9. \ No newline at end of file diff --git a/en/star/Van_Maanenova_hviezda.md b/en/star/Van_Maanenova_hviezda.md deleted file mode 100644 index 521fcbe1e..000000000 --- a/en/star/Van_Maanenova_hviezda.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Van Maanenova hviezda -constellation: Psc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.786644 ---- diff --git a/en/star/W_a_X_Sgr.md b/en/star/W_a_X_Sgr.md deleted file mode 100644 index d98afc453..000000000 --- a/en/star/W_a_X_Sgr.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: W a X Sgr -constellation: Sgr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:39:47.585091 ---- -cepheid, which change their brightness with a weekly period from fourth to fifth magnitude. X SGR lies almost on the boundary with the constellation Hadonose. It reaches 4.3mag at maximum and 4.9mag at minimum. Its period is 7.012 days. W SGR fluctuates between 4.3mag and 5mag with a period of 7.595 days. \ No newline at end of file diff --git a/en/star/Wolf_359.md b/en/star/Wolf_359.md deleted file mode 100644 index 3101d358e..000000000 --- a/en/star/Wolf_359.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Wolf 359 -constellation: Leo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:42:02.875256 ---- -a faint star with a brightness of 13.7mag, named in honour of Max Wolf, working at Heidelburg University in the early 20th century, who discovered its proper motion. It moves 4.71" across the sky every year. One reason for this apparent movement is its proximity to us. It lies at a distance of just 7.86 light years from the Sun, making it our third closest star after Proxima Centauri and Barnard's Star in Hadonos. \ No newline at end of file diff --git a/en/star/Wolf_457.md b/en/star/Wolf_457.md deleted file mode 100644 index 0e1e30ef6..000000000 --- a/en/star/Wolf_457.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Wolf 457 -constellation: Dra -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:26:44.522159 ---- diff --git a/en/star/Z_Cam.md b/en/star/Z_Cam.md deleted file mode 100644 index 267dbac87..000000000 --- a/en/star/Z_Cam.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Z Cam -constellation: Cam -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 19:11:49.037725 ---- - a cataclysmic variable star that jumps every two to three weeks from a minimum of about 13mag to a maximum of magnitude 9.6mag. But that's where its similarity to other variable stars of this type ends. In fact, its magnitude can stop in the declining phase and stay at its mean brightness for a very long time. It stays like this for several months before its magnitude starts to increase again - so the star fades. \ No newline at end of file diff --git a/en/star/Z_Cha.md b/en/star/Z_Cha.md deleted file mode 100644 index 0b3a5cf28..000000000 --- a/en/star/Z_Cha.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Z Cha -constellation: Cha -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-24 14:47:45.100294 ---- -a fainter variable star that only shines as a 16.2mag star at its minimum, so we can only see it in a large telescope. But every three to four months it brightens sharply and within a few hours its brightness rises to 11.5mag. For a few days, we'll see it in a 150mm telescope. \ No newline at end of file diff --git a/en/star/h3945.md b/en/star/h3945.md deleted file mode 100644 index 5441978d8..000000000 --- a/en/star/h3945.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: h3945 -constellation: CMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:50:48.102766 ---- -winter Albireo or Alamak. A beautiful double star consisting of an orange 4.8mag and a blue 6.8mag component. At a distance of 26.6" it can be resolved with a small telescope. \ No newline at end of file diff --git a/en/star/hr1010.md b/en/star/hr1010.md deleted file mode 100644 index 66ae132dd..000000000 --- a/en/star/hr1010.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ζ Ret -constellation: Ret -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-08 14:47:27.641555 ---- -an optical binary whose components are similar to our sun. Their brightnesses are 5.2mag and 5.5mag. At a distance of about 39 light years, we can distinguish them with the naked eye. \ No newline at end of file diff --git a/en/star/hr1017.md b/en/star/hr1017.md deleted file mode 100644 index 31fe1afff..000000000 --- a/en/star/hr1017.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Algenib (α Per) -constellation: Per -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.647029 ---- diff --git a/en/star/hr1084.md b/en/star/hr1084.md deleted file mode 100644 index d618ab38d..000000000 --- a/en/star/hr1084.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ε Eri -constellation: Eri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.547302 ---- diff --git a/en/star/hr1175.md b/en/star/hr1175.md deleted file mode 100644 index 9b5846286..000000000 --- a/en/star/hr1175.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Ret -constellation: Ret -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-08 14:46:12.471846 ---- -the main component has a magnitude of 3.85mag and at a distance of 14" is its companion with a magnitude of 8.1mag. It lies at a distance of 100 light years. \ No newline at end of file diff --git a/en/star/hr1203.md b/en/star/hr1203.md deleted file mode 100644 index c9644b696..000000000 --- a/en/star/hr1203.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ζ Per -constellation: Per -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.832682 ---- diff --git a/en/star/hr1208.md b/en/star/hr1208.md deleted file mode 100644 index 263e81cc8..000000000 --- a/en/star/hr1208.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: γ Hyi -constellation: Hyi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.530529 ---- diff --git a/en/star/hr1212.md b/en/star/hr1212.md deleted file mode 100644 index ef36b1528..000000000 --- a/en/star/hr1212.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: 32 Eri -constellation: Eri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.074548 ---- diff --git a/en/star/hr1220.md b/en/star/hr1220.md deleted file mode 100644 index 91cf3a164..000000000 --- a/en/star/hr1220.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ε Per -constellation: Per -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.199632 ---- diff --git a/en/star/hr1239.md b/en/star/hr1239.md deleted file mode 100644 index a68f24f1c..000000000 --- a/en/star/hr1239.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: λ Tau -constellation: Tau -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 09:55:20.993737 ---- -an occultation variable star of the Algol type, with magnitude variations from 3.3 to 3.8 over a period of 3.95 days. Suitable comparison stars are γ (3.6mag), μ (4.3 m), ο (3.6mag), and ζ (3.7mag). λ Tau is actually much more luminous than Algol, but is located at a much greater distance (480 light years). Its light changes were first observed by J. Baxendell of England in 1848. \ No newline at end of file diff --git a/en/star/hr126.md b/en/star/hr126.md deleted file mode 100644 index fb1248318..000000000 --- a/en/star/hr126.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Tuc -constellation: Tuc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-24 07:42:05.476646 ---- -not only an optical but also a physical binary star. Two almost equally bright components of 4.4mag and 4.5mag are separated by 27.1", so we can distinguish them in a good binocular. Both are still double, which we only notice in binoculars. At a distance of 9.3' to the southeast, we can additionally observe a third component of 5.1mag brightness, which is actually also a close binary. \ No newline at end of file diff --git a/en/star/hr1298.md b/en/star/hr1298.md deleted file mode 100644 index 25c352bcb..000000000 --- a/en/star/hr1298.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Keid (ο2 Eri) -constellation: Eri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.579056 ---- diff --git a/en/star/hr1311.md b/en/star/hr1311.md deleted file mode 100644 index 9470e668a..000000000 --- a/en/star/hr1311.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 47 Tau -constellation: Tau -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 09:55:49.629906 ---- -a tight double star even for binoculars with a 200mm lens diameter. Up to 200x magnification will show two yellow stars that have a brightness of 4.9mag and 7.4mag and lie only 1.1" apart. \ No newline at end of file diff --git a/en/star/hr1326.md b/en/star/hr1326.md deleted file mode 100644 index d7fbf614d..000000000 --- a/en/star/hr1326.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: α Hor -constellation: Hor -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.368733 ---- diff --git a/en/star/hr1336.md b/en/star/hr1336.md deleted file mode 100644 index fa0058c82..000000000 --- a/en/star/hr1336.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Ret -constellation: Ret -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-08 14:45:11.805870 ---- -the brightest star in the constellation with an apparent brightness of 3.36mag. It belongs to spectral class G6 and is faintly yellowish. At an angular distance of 48.5" is a 12mag companion. It is 163 light years away. \ No newline at end of file diff --git a/en/star/hr1348.md b/en/star/hr1348.md deleted file mode 100644 index 543eadd42..000000000 --- a/en/star/hr1348.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: φ Tau -constellation: Tau -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 09:56:13.752435 ---- -consists of two stars 5mag and 8.4mag at a mutual distance of 52.1". A good triad is sufficient to distinguish the two components. In a small telescope we can see the yellow and blue shades respectively. \ No newline at end of file diff --git a/en/star/hr1355.md b/en/star/hr1355.md deleted file mode 100644 index ef313d660..000000000 --- a/en/star/hr1355.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Ret -constellation: Ret -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-08 14:46:45.000162 ---- -A binary star consisting of a main component of 4.4mag and a faint companion of 12.5mag, which lies at a distance of 13.7". The system lies at a distance of 60 light years. \ No newline at end of file diff --git a/en/star/hr1412.md b/en/star/hr1412.md deleted file mode 100644 index ab345b8e5..000000000 --- a/en/star/hr1412.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: θ Tau -constellation: Tau -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 09:54:51.458049 ---- -a wide binary star in the Hyades visible to the naked eye. It consists of two bright components 3.6mag and 4mag at a distance of 337". Its brighter component is white, the guide is orange. They are 15 light years apart, but it is quite likely that they share a common origin. \ No newline at end of file diff --git a/en/star/hr1457.md b/en/star/hr1457.md deleted file mode 100644 index ef84a5c7b..000000000 --- a/en/star/hr1457.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Aldebaran (α Tau) -constellation: Tau -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 09:54:25.010444 ---- -the brightest star in the constellation (0.85mag). An orange giant of spectral class K5, its name is of Arabic origin and means "next" - because it rises after the Pleiades and follows them in their daily movement from east to west. It is 65 light years away from us and represents the eye of Taurus in the sky. Its actual luminosity is 125 times that of the Sun. It projects quite randomly into the open star cluster of Hyades, which actually lies beyond it. diff --git a/en/star/hr1465.md b/en/star/hr1465.md deleted file mode 100644 index 78f578c4a..000000000 --- a/en/star/hr1465.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Dor -constellation: Dor -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:14:22.786832 ---- -the brightest star in the constellation has an apparent brightness of 3.47mag. In reality, it is a close binary because 77.7" from the main component is a companion of 9.8mag brightness. It lies at a distance of 176 light years. \ No newline at end of file diff --git a/en/star/hr15.md b/en/star/hr15.md deleted file mode 100644 index b711d9f78..000000000 --- a/en/star/hr15.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Sirrah -constellation: Peg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.210835 ---- diff --git a/en/star/hr1502.md b/en/star/hr1502.md deleted file mode 100644 index 3030cea5a..000000000 --- a/en/star/hr1502.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Cae -constellation: Cae -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 18:20:01.546359 ---- -the brightest star in the constellation, although it only reaches 4.52mag. In fact, it is a double star, with a 12.4mag companion at a distance of 6.6" from the main component. However, we need a larger telescope to verify this. The system is 66 light years away. \ No newline at end of file diff --git a/en/star/hr154.md b/en/star/hr154.md deleted file mode 100644 index 5862529a0..000000000 --- a/en/star/hr154.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: π Andromedae -constellation: And -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:07:31.617236 ---- -a double star (stars are 4.4mag and 8.6mag, angular distance 35.9'') resolvable with a small telescope with a 6 cm diameter lens. The main component reaches an absolute magnitude of -1.1, is 170 times brighter than the Sun, and lies at a distance of 600 light years. In a telescope with a 200mm diameter objective lens, it appears as a bright white star with a dull bluish guide. A faint 13th magnitude star is also projected into the neighbourhood. \ No newline at end of file diff --git a/en/star/hr1542.md b/en/star/hr1542.md deleted file mode 100644 index 3afe9d0be..000000000 --- a/en/star/hr1542.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Cam -constellation: Cam -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 19:07:49.486705 ---- -appears as a 4.3-mag star in the sky. But in reality, this blue giant of spectral class O is 620 000 times brighter than the Sun. It's about 6,000,000 light-years away. \ No newline at end of file diff --git a/en/star/hr1563.md b/en/star/hr1563.md deleted file mode 100644 index f1b018913..000000000 --- a/en/star/hr1563.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ι Pic -constellation: Pic -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.634865 ---- diff --git a/en/star/hr1603.md b/en/star/hr1603.md deleted file mode 100644 index 3807a20ca..000000000 --- a/en/star/hr1603.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Cam -constellation: Cam -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 19:07:21.923114 ---- -the brightest star in the constellation, has an apparent brightness of 4.22mag. This yellow giant of spectral class G0 is 870 light years away and shines 1,600 times brighter than our Sun. The surface temperature is 30,000 Kelvin. \ No newline at end of file diff --git a/en/star/hr1605.md b/en/star/hr1605.md deleted file mode 100644 index 03b0d9ca9..000000000 --- a/en/star/hr1605.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Al Anz (ε Aur) -constellation: Aur -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:47:32.918024 ---- -one of the three stars of the crucifixes, which is one of the remarkable occultation variables of the Algol type. It consists of a bright white supergiant 4 billion km across, 37,000 times brighter than the Sun, and a dark companion, but visually unobservable. The two stars are in mutual orbit. Every 27 years - 9,883 days - the dark component passes in front of the supergiant and obscures much of its light, making the star ε Aur much dimmer in our sky - from 3.1mag to 3.8mag. This darkening lasts for months - about 190 days, then the star stays at minimum for about half a year, and grows from minimum to maximum in another 190 days. This suggests that the guide must be surrounded by a dark cloud of gas and dust. The last such occultation occurred in 2009. It has one of the longest periods among known occultation variables. \ No newline at end of file diff --git a/en/star/hr1612.md b/en/star/hr1612.md deleted file mode 100644 index 6e081e285..000000000 --- a/en/star/hr1612.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Sadatoni (ζ Aur) -constellation: Aur -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:48:01.950914 ---- -another occultation variable star from the crust, with a magnitude change from 3.9mag to 4.2mag over a period of 2.66 years - 972.18 days, the second longest known period. The decline in brightness from maximum to minimum, or rise from minimum to maximum, lasts only a few days, the star remaining at minimum for 38 days. The main component is red, the minor component is blue. Sometimes bright blue stars come to us through the outer layers of the red supergiant, producing interesting spectroscopic phenomena. \ No newline at end of file diff --git a/en/star/hr1629.md b/en/star/hr1629.md deleted file mode 100644 index 3625b070a..000000000 --- a/en/star/hr1629.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: η Men -constellation: Men -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.105569 ---- diff --git a/en/star/hr1652.md b/en/star/hr1652.md deleted file mode 100644 index f06da4b73..000000000 --- a/en/star/hr1652.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ Cae -constellation: Cae -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 18:20:21.015175 ---- -a binary star only distinguishable with a larger telescope. The main yellow-orange star with a brightness of 4.7mag has a guide star with a brightness of 8.5mag at a distance of 2.9 arc seconds. \ No newline at end of file diff --git a/en/star/hr167.md b/en/star/hr167.md deleted file mode 100644 index b8b15b5b2..000000000 --- a/en/star/hr167.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: 55 Psc -constellation: Psc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.952990 ---- diff --git a/en/star/hr1677.md b/en/star/hr1677.md deleted file mode 100644 index 33cfd25c1..000000000 --- a/en/star/hr1677.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: β Men -constellation: Men -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.167058 ---- diff --git a/en/star/hr168.md b/en/star/hr168.md deleted file mode 100644 index 24366eb60..000000000 --- a/en/star/hr168.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Schedar (α Cassiopeiae) -constellation: Cas -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:10:50.892772 ---- -this orange star 228 light-years away is 676 times brighter than our Sun, but only appears as a 2.23-mag constant in the sky (the magnitude actually varies by a few tenths). \ No newline at end of file diff --git a/en/star/hr1705.md b/en/star/hr1705.md deleted file mode 100644 index 2300c0e52..000000000 --- a/en/star/hr1705.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: κ Lep -constellation: Lep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:48:00.636273 ---- -this binary is made up of 4.5mag and 7.4mag components, which lie at an angular separation of 2.6". To resolve them, we need a telescope with a lens diameter of at least 15 cm. At about 115x magnification, both components appear white. It is only in a larger telescope that the guide becomes blue. \ No newline at end of file diff --git a/en/star/hr1706.md b/en/star/hr1706.md deleted file mode 100644 index 48c283902..000000000 --- a/en/star/hr1706.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 14 Aur -constellation: Aur -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:48:28.611785 ---- - triple star, the main, bright yellow component with a brightness of 5.2mag has a pale blue companion with a brightness of 7.4mag at a distance of 14.6 arc seconds. In a larger telescope, a third, fainter companion is added, located in a sparse star field. \ No newline at end of file diff --git a/en/star/hr1708.md b/en/star/hr1708.md deleted file mode 100644 index bc1fa67a3..000000000 --- a/en/star/hr1708.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Capella (α Aur) -constellation: Aur -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:46:20.927878 ---- -the brightest star in the constellation and the sixth brightest star in the sky (0.1 mag). It does not set in our area. It is the northernmost in the Winter Hexagon of bright stars. With the naked eye, we can see its yellow hue. It is 43 light years away and its true luminosity is 160 times that of the Sun. It is one of the most famous spectroscopic binaries that orbit around a common point, with an orbit that lasts 108 days. In terms of spectrum and surface temperature, they are comparable to our Sun. The masses reach 2.5 and 2.5 times that of the Sun, respectively, and one of the stars is 78 and 72 times more luminous than the Sun. \ No newline at end of file diff --git a/en/star/hr1713.md b/en/star/hr1713.md deleted file mode 100644 index afd9be82e..000000000 --- a/en/star/hr1713.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Rigel (β Ori) -constellation: Ori -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:54:13.610367 ---- -is usually the brightest star in the constellation, only occasionally surpassed by Betelgeuse during its peak. At 0.14mag, it is the seventh brightest star in the sky. It is a supernova of spectral type B8, so its blue-white colour can be clearly seen with the naked eye. Rigel is 78 times bigger and 12 000 times brighter than our Sun and lies 860 light years away. \ No newline at end of file diff --git a/en/star/hr1829.md b/en/star/hr1829.md deleted file mode 100644 index e262cf054..000000000 --- a/en/star/hr1829.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Nihal (β Lep) -constellation: Lep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:47:07.074593 ---- -the triple stars. For a star with a brightness of 2.8mag, there are two components at a distance of 2.5" and 64", both with a brightness of 11mag. The more distant component is only an optical guide. The main star is 160 light years away. \ No newline at end of file diff --git a/en/star/hr183.md b/en/star/hr183.md deleted file mode 100644 index e675c3dda..000000000 --- a/en/star/hr183.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ξ Phe -constellation: Phe -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.020034 ---- diff --git a/en/star/hr1852.md b/en/star/hr1852.md deleted file mode 100644 index d4f04f25f..000000000 --- a/en/star/hr1852.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Mintaka (δ Ori) -constellation: Ori -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:55:37.471347 ---- -the true blue-white star of the belt near the celestial equator. This is one of the easiest pairs to distinguish - a telescope with a 5 cm diameter lens will suffice. We'll see the pale blue 6.9mag companion next to the main component at a distance of 52.6". This is probably a real star pair, even though the components are half a light year apart. So their mutual orbital period could be a million years. The system lies at a distance of 2,350 light years. The main component is also a variable star, but with a very small change in brightness (about 2.2 mag). \ No newline at end of file diff --git a/en/star/hr1865.md b/en/star/hr1865.md deleted file mode 100644 index a6e92ff23..000000000 --- a/en/star/hr1865.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Arneb (α Lep) -constellation: Lep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:46:37.142187 ---- -the brightest star in the constellation (2.58mag), 2200 light years away. It is a supergiant 32,000 times brighter than the Sun. At an angular distance of 36" it contains a faint 11mag guide star. \ No newline at end of file diff --git a/en/star/hr1879.md b/en/star/hr1879.md deleted file mode 100644 index 87d7f973a..000000000 --- a/en/star/hr1879.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: λ Ori -constellation: Ori -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:56:30.122062 ---- -the white companions have a brightness of 3.5mag and 5.6mag, their mutual spacing is 4.4". The other two, bluish companions lie 28" and 78" respectively from this pair. λ Ori denotes the head of Orion and forms an interesting triangle with π-1 and π-2 Ori. Both reach 4th sidereal magnitude. \ No newline at end of file diff --git a/en/star/hr188.md b/en/star/hr188.md deleted file mode 100644 index b4e48e5c5..000000000 --- a/en/star/hr188.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Deneb Kaitos (β Cet) -constellation: Cet -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 18:15:06.650587 ---- -with a brightness of 2.04mag is the brightest star in the constellation. But when the long period variable star Mira Ceti is at its maximum, it becomes the brightest star in the constellation. Deneb Kaitos is pointed at the conjunction of the stars Alpheratz and Gamma Pegasi from the Pegasus square. It is sometimes confused with the star Fomalhaut, but is magnitude fainter compared to it. It is 96 light years away. \ No newline at end of file diff --git a/en/star/hr1899.md b/en/star/hr1899.md deleted file mode 100644 index 80d8f8a9d..000000000 --- a/en/star/hr1899.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ι Ori -constellation: Ori -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:56:06.902242 ---- -nice triple star suitable for small telescopes. Next to the main white component (2.8mag) lies a pale blue 7.3mag guide at a distance of 11.3". Another, reddish companion 11mag is observed at a distance of 50" from this pair. The trier shows the even wider binary Struve 747 nearby, which is made up of bright 4.8 and 5.7mag components. \ No newline at end of file diff --git a/en/star/hr191.md b/en/star/hr191.md deleted file mode 100644 index 3bfb4e289..000000000 --- a/en/star/hr191.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: η Phe -constellation: Phe -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.901191 ---- diff --git a/en/star/hr1914.md b/en/star/hr1914.md deleted file mode 100644 index 129243022..000000000 --- a/en/star/hr1914.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 26 Aur -constellation: Aur -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:48:57.960120 ---- - triple star, the AB pair (6mag) is too close together for resolution (0.2") for amateur telescopes, but the third component (8mag) with it makes a nice contrast of unequally bright yellow and blue stars at a distance of 12.4". \ No newline at end of file diff --git a/en/star/hr1922.md b/en/star/hr1922.md deleted file mode 100644 index 6491554e5..000000000 --- a/en/star/hr1922.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Dor -constellation: Dor -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:15:07.042098 ---- -A variable Cepheid that reaches a maximum brightness of 3.8mag and decreases to 4.6mag at minimum with a period of 9.84 days. This yellow-white giant is about 1,000 light-years away. A suitable comparison star is Delta Dor, which reaches a brightness of 4.35 mag. \ No newline at end of file diff --git a/en/star/hr1931.md b/en/star/hr1931.md deleted file mode 100644 index e7eb41c16..000000000 --- a/en/star/hr1931.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: σ Ori -constellation: Ori -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:57:17.186221 ---- -already with a telescope with a 5 cm objective diameter we can detect two guides in the main white component 3.81mag. The first 6mag lies at a distance of 41", the second 7mag is separated by a distance of 13" . In a telescope with a lens diameter of about 15 cm, a companion 10mag is added at a distance of 11". Another 6mag companion lies within 0.2" of the main component, but it is the only one physically related to the main component. \ No newline at end of file diff --git a/en/star/hr1948.md b/en/star/hr1948.md deleted file mode 100644 index b5c4ede6d..000000000 --- a/en/star/hr1948.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alnitak (ζ Ori) -constellation: Ori -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:55:07.438010 ---- -the left star of Orion's belt is actually a triple star. Near the main component of 1.9mag is a 4.2mag companion at a distance of 2.7", and at an angular distance of 57" is another 9mag star that probably only projects into the vicinity of Alnitak. All components have a blue-white hue. \ No newline at end of file diff --git a/en/star/hr1953.md b/en/star/hr1953.md deleted file mode 100644 index ac80f7218..000000000 --- a/en/star/hr1953.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: γ Men -constellation: Men -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.891882 ---- diff --git a/en/star/hr1956.md b/en/star/hr1956.md deleted file mode 100644 index daf89d7af..000000000 --- a/en/star/hr1956.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Phakt (α Col) -constellation: Col -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:36:06.382039 ---- -the brightest star in the constellation. The main pale blue component 2.64mag has a companion 11mag at a distance of 13.5 arc seconds, which we can see with a 100 mm telescope. The system is 145 light years away. \ No newline at end of file diff --git a/en/star/hr1983.md b/en/star/hr1983.md deleted file mode 100644 index b79e0f618..000000000 --- a/en/star/hr1983.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ Lep -constellation: Lep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:47:35.226621 ---- -this binary splits into two components in the binocular, one reaching 3.7mag (yellow) and the other 6.3mag (orange). The components are 96.3" apart, separated by about 29 light years from Earth. The star belongs to the motion cluster of the Big Dipper. \ No newline at end of file diff --git a/en/star/hr1992.md b/en/star/hr1992.md deleted file mode 100644 index 3e824d9fa..000000000 --- a/en/star/hr1992.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 29 Cam -constellation: Cam -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 19:10:58.810332 ---- -a double star suitable for 100 mm telescope. That it is a double star is obvious at 100x magnification. It appears as an unequally bright (6.5mag, 9.5mag) and contrasting pair of yellow and pale blue components. Their mutual distance is 25.1". \ No newline at end of file diff --git a/en/star/hr1996.md b/en/star/hr1996.md deleted file mode 100644 index a875e51e1..000000000 --- a/en/star/hr1996.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: μ Col -constellation: Col -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:37:59.475012 ---- -a very interesting star, one of a trio of stars that emerge from the constellation Orion. Together with 53 Ari and AE Aur, it apparently once formed a star system in the constellation Orion, the fourth component of which exploded as a supernova 2-3 billion years ago, disrupting the stability of the other three and causing them to gradually move away from their original location. In our galaxy, μ Col is moving at around 100 km/s. \ No newline at end of file diff --git a/en/star/hr2020.md b/en/star/hr2020.md deleted file mode 100644 index c86bf60b9..000000000 --- a/en/star/hr2020.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: β Pic -constellation: Pic -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.876361 ---- diff --git a/en/star/hr2061.md b/en/star/hr2061.md deleted file mode 100644 index a25e6fb59..000000000 --- a/en/star/hr2061.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Betelgeuse (α Ori) -constellation: Ori -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:54:38.243093 ---- -this luminous red giant is a semi-regular variable star whose brightness varies between 0.4mag and 1.3mag over a period of about 5.7 years. However, it is more orange in colour in the binocular. Betelgeuse is one of the largest stars visible to the naked eye. If it were at the position of the Sun, its edge would extend to the asteroid belt. It lies 500-600 light years away. \ No newline at end of file diff --git a/en/star/hr2095.md b/en/star/hr2095.md deleted file mode 100644 index e17cf81de..000000000 --- a/en/star/hr2095.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: θ Aur -constellation: Aur -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:46:43.352731 ---- -triple constellation, the 2.6mag and 7.1mag brightness components lie 3.6" apart. There is also a third star in the field of view at a distance of 45". To resolve the entire system, we need a telescope with an 8 cm objective diameter. \ No newline at end of file diff --git a/en/star/hr2176.md b/en/star/hr2176.md deleted file mode 100644 index d73ddeba8..000000000 --- a/en/star/hr2176.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 41 Aur -constellation: Aur -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:49:25.054681 ---- -a nice pair of white (6.3mag) and pale blue (7mag) components at 7.7" resolved in a small telescope. The environment is completed by the variable star 46 Aur, 3 degrees away at VSV, which is clearly orange. \ No newline at end of file diff --git a/en/star/hr219.md b/en/star/hr219.md deleted file mode 100644 index 480eca6d1..000000000 --- a/en/star/hr219.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Achird (η Cassiopeiae) -constellation: Cas -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:11:59.909995 ---- -a well-known binary star discovered in 1779 by William Herschel. The yellow, golden star (3.7mag) has a guide star of brightness 7.4mag with a red, purple tinge at a distance of 13" (the distance varies from 5" to 16" in period), which orbits it in 526 years. We can resolve the double star in a 6 cm telescope. \ No newline at end of file diff --git a/en/star/hr2216.md b/en/star/hr2216.md deleted file mode 100644 index 3bbf5bbf3..000000000 --- a/en/star/hr2216.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Tejat Prior (η Gem) -constellation: Gem -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:13:55.251317 ---- -red giant, a bright semi-regular variable star with magnitude variations from 3.1 to 3.9 over a period of about 223 days. At a distance of 1.4", the guide has a magnitude of 8.8. A good comparison star is μ Gem. It lies at a distance of 700 light years. \ No newline at end of file diff --git a/en/star/hr2261.md b/en/star/hr2261.md deleted file mode 100644 index cf48b59c8..000000000 --- a/en/star/hr2261.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: α Men -constellation: Men -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.818578 ---- diff --git a/en/star/hr2293.md b/en/star/hr2293.md deleted file mode 100644 index 1bc56c64d..000000000 --- a/en/star/hr2293.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 5 Lyn -constellation: Lyn -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:52:20.717778 ---- -triple constellation, even in a smaller telescope, is a nice, wide pair of yellow 5.3mag and blue 9.8mag components that lie 31.4" apart. A third component of 7.9mag lies at a distance of 96". The binary 6 Lyn and two other wide pairs lie nearby. The one that lies one degree northeast of 5 Lyn is made up of an orange and blue component, the other is made up of two white components. \ No newline at end of file diff --git a/en/star/hr2298.md b/en/star/hr2298.md deleted file mode 100644 index 5bae7dc4f..000000000 --- a/en/star/hr2298.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Mon -constellation: Mon -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 10:12:43.137174 ---- -the main star with a brightness of 4.5mag has a guide star with a brightness of 6.5mag at a distance of 13.4", which we can find with a smaller telescope. Both components are yellow. At a distance of 93.7" from them, we can detect a pale blue companion of 12.7mag with a larger telescope. \ No newline at end of file diff --git a/en/star/hr2326.md b/en/star/hr2326.md deleted file mode 100644 index 5278592ce..000000000 --- a/en/star/hr2326.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Canopus (α Car) -constellation: Car -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 09:59:41.769903 ---- -the main star of the constellation, but also once of the entire Argo ship as α Argus, whose helm it marked. Being at the very northwestern edge of the constellation, as an orange star it could be seen from as far north as North Africa, low over the southern horizon. During the local winter, it culminates about 20 minutes before the actual spread from the Big Dog. Canopus is a yellow supergiant of spectral class FO, its brightness of -0.8mag making it the second brightest star in the sky after the spread. It is 313 light-years away from the Sun and is 200,000 times more luminous by contrast. Interestingly, it lies quite far from the ecliptic, which is why most interplanetary satellites use it to navigate in space. \ No newline at end of file diff --git a/en/star/hr2356.md b/en/star/hr2356.md deleted file mode 100644 index f7c40de9c..000000000 --- a/en/star/hr2356.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Mon -constellation: Mon -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 10:13:05.317779 ---- -the brightest star in the constellation has an apparent brightness of 3.95mag. It is one of the magnificent triple stars discovered in 1781 by W. Herschel, all of whose blue-white components can be distinguished even with small telescopes as a tiny triangle. The two components of brightness 4.7mag and 5.2mag are located 7.3" apart. The 6.1mag guide lies at a distance of 2.8" from the first component. The system is about 700 light years away. With a larger telescope, we can still detect a 12mag star at a distance of 25.9". This entire system is referred to as 11 Mon. \ No newline at end of file diff --git a/en/star/hr2451.md b/en/star/hr2451.md deleted file mode 100644 index 96c5e30c3..000000000 --- a/en/star/hr2451.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ν Pup -constellation: Pup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 12:00:57.155167 ---- -an easily resolved binary only 26' NE of σ Puppis. The components of this pair have brightnesses of 4.7mag and 5.1mag and a mutual separation of 4'. \ No newline at end of file diff --git a/en/star/hr2470.md b/en/star/hr2470.md deleted file mode 100644 index f97dbfe59..000000000 --- a/en/star/hr2470.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 12 Lyn -constellation: Lyn -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:51:57.490919 ---- -a physical binary star made up of relatively equally bright components - 5.4mag and 6mag. They are 1.8" apart and have an orbital period of 907 years. At a distance of about 8.5" from the brighter component is another companion with a brightness of 7.5mag. \ No newline at end of file diff --git a/en/star/hr2491.md b/en/star/hr2491.md deleted file mode 100644 index 27902f5c0..000000000 --- a/en/star/hr2491.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Sírius (α CMa) -constellation: CMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:46:28.971142 ---- -the brightest star in the sky, known to all ancient peoples. Orion's belt extends downwards towards Sirius. There, near the horizon, we see, especially on cold winter nights, a bright blue-white star twinkling with the action of the restless air in the atmosphere. After all, the Greek word "Sirios" already means flickering, sparkling. Sirius has a brightness of -1.5mag, but it's not particularly bright compared to other stars. In fact, it owes everything to its relatively close proximity to us - 8.7 light-years - which puts it fifth in the list of our nearest stars (if you don't count the guide stars). It has 23 times the luminosity, 1.8 times the diameter and 2.35 times the mass of our Sun. Its surface temperature of 10,000 K causes its blue-white colouration. \ No newline at end of file diff --git a/en/star/hr2550.md b/en/star/hr2550.md deleted file mode 100644 index 5cacfdd34..000000000 --- a/en/star/hr2550.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: α Pic -constellation: Pic -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.062616 ---- diff --git a/en/star/hr2564.md b/en/star/hr2564.md deleted file mode 100644 index 0ce87494a..000000000 --- a/en/star/hr2564.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 38 Gem -constellation: Gem -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:15:20.840611 ---- -The companions have a brightness of 4.7mag and 7.7mag and orbit each other once every 3,190 years or so. At the turn of the century, they were about 7.1" apart, which makes the components comfortably separated with a telescope with an 8 cm diameter lens. One is yellow, the other light blue. \ No newline at end of file diff --git a/en/star/hr258.md b/en/star/hr258.md deleted file mode 100644 index 5bc6cd8a7..000000000 --- a/en/star/hr258.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 36 Andromedae -constellation: And -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:07:21.111345 ---- - a close binary (6mag and 6.4mag components at 0.6"- 1.4" separation over 165 years) that is a test for larger amateur telescopes. It is 124 light years away. The main component is many times brighter than our Sun. The guide, on the other hand, is very similar to the Sun. It is of the same spectral type and has the same colour - a nice yellow. \ No newline at end of file diff --git a/en/star/hr2588.md b/en/star/hr2588.md deleted file mode 100644 index 5cabac9bf..000000000 --- a/en/star/hr2588.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 17 CMa -constellation: CMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:49:45.713223 ---- -very nice multiple star even for small telescope! Low magnification shows a beautiful wide triple star with a white 5.8mag main component and two orange companions forming a right triangle. The companion 9.5mag and the binary π Canis Majoris are seen in the same field of view. \ No newline at end of file diff --git a/en/star/hr2593.md b/en/star/hr2593.md deleted file mode 100644 index c3d9602bc..000000000 --- a/en/star/hr2593.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: μ CMa -constellation: CMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:48:56.725849 ---- - in a small telescope, an unevenly bright pair of stars in contact with each other, a sparkling contrast of orange and blue. In a larger telescope, we can separate them with 175x magnification. The yellow component has a brightness of 5.3mag, the blue component of 8.6mag lies 3" apart. The two 10mag companions are a little further away. \ No newline at end of file diff --git a/en/star/hr2618.md b/en/star/hr2618.md deleted file mode 100644 index f5c7f1f33..000000000 --- a/en/star/hr2618.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Adara (ε CMa) -constellation: CMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:47:31.420966 ---- -a binary whose 8.1mag guide lies at a distance of 7.5" from the main component, which has a brightness of 1.5mag. Because of the large difference in their brightnesses, we will need a telescope with a lens diameter of at least 15 cm to resolve them. \ No newline at end of file diff --git a/en/star/hr264.md b/en/star/hr264.md deleted file mode 100644 index c3e4f4f91..000000000 --- a/en/star/hr264.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Cih (γ Cassiopeiae) -constellation: Cas -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:11:29.427253 ---- -The white giant, the star in the middle of the letter "W", is the brightest in this cluster. It's about 34,000 times brighter than the sun and 550 light years away. Using a larger amateur telescope, we can detect an 11-magnitude guide at a distance of 2.3". \ No newline at end of file diff --git a/en/star/hr2650.md b/en/star/hr2650.md deleted file mode 100644 index e67702380..000000000 --- a/en/star/hr2650.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Mekbuda (ζ Gem) -constellation: Gem -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:14:59.981504 ---- -one of the brightest Cepheids in the sky: the main yellow star varies its brightness from 3.6mag to 4.1mag with a period of 10.15 days. Suitable comparison stars are κ (3.57mag) and υ Gem (4.07mag). One guide is located at a distance of 96" and has a brightness of 8mag, the other 11mag is observed 87" away. However, they are only optically companions. Mekbuda pulses from a distance of 1120 light years. \ No newline at end of file diff --git a/en/star/hr2671.md b/en/star/hr2671.md deleted file mode 100644 index 29559c981..000000000 --- a/en/star/hr2671.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Gem -constellation: Gem -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:15:44.662825 ---- -a variable star of the type Mira Ceti, its brightness varies between 6-14mag over a period of 370 days. It lies close to the star δ Gem. \ No newline at end of file diff --git a/en/star/hr2736.md b/en/star/hr2736.md deleted file mode 100644 index 72611ffb5..000000000 --- a/en/star/hr2736.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ Vol -constellation: Vol -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-24 07:38:53.958209 ---- -an attractive binary for small telescopes, with brightness components of 3.8mag and 5.7mag lying at a distance of 13.6". They are orange and yellow in colour. \ No newline at end of file diff --git a/en/star/hr2742.md b/en/star/hr2742.md deleted file mode 100644 index 520e42e6b..000000000 --- a/en/star/hr2742.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: VZ Cam -constellation: Cam -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 19:09:57.821311 ---- -a semi-regular M-type variable star, appearing bright red when observed through a binocular. It shows small, irregular magnitude changes, from 4.8mag to 5.2mag with a mean period of about 24 days. Because of its proximity to the celestial pole, it can be observed throughout the year from more northerly latitudes. \ No newline at end of file diff --git a/en/star/hr2748.md b/en/star/hr2748.md deleted file mode 100644 index 6bf2e2f9d..000000000 --- a/en/star/hr2748.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: L2 Puppis -constellation: Pup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 12:01:44.872031 ---- -a bright long-period variable star belonging to the Myriad group, one of the brightest red variable stars, whose brightness varies between 2.6mag and 6.2mag over a period of 141 days. At its maximum, it is therefore very visible from illuminated areas, but at its minimum it falls to the limit of naked-eye visibility. \ No newline at end of file diff --git a/en/star/hr2777.md b/en/star/hr2777.md deleted file mode 100644 index b32693dd2..000000000 --- a/en/star/hr2777.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Wasat (δ Gem) -constellation: Gem -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:14:36.959097 ---- -a binary star distinguishable with a small telescope. The main star has a brightness of 3.5mag and the companion 8.2mag, with an orbital period of about 1,200 years. In 1985, the companion was 6" away from the main star, so it could be observed with a telescope with a 6 cm diameter objective lens. By 2000, their mutual distance had been reduced to 5.8". Even so, this is no problem for a 200 mm telescope, in which we can see their yellow or light blue color. \ No newline at end of file diff --git a/en/star/hr2782.md b/en/star/hr2782.md deleted file mode 100644 index f7d3ba6e0..000000000 --- a/en/star/hr2782.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: τ CMa -constellation: CMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:48:13.379538 ---- -This beautiful multiple star is observable with a small telescope inside the open cluster NGC 2362. It lies in a beautiful environment crowded with faint stars. The main component is yellow 4.4mag, the companion is bluish 10.5mag. It lies at a distance of 8.2". \ No newline at end of file diff --git a/en/star/hr2784.md b/en/star/hr2784.md deleted file mode 100644 index dfd070f6c..000000000 --- a/en/star/hr2784.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 19 Lyn -constellation: Lyn -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:52:43.011607 ---- -this optical binary can be easily resolved with a small telescope. The two stars, one 5.6mag and the other 6.5mag, are 14.8" apart. The first is yellow-white, the second light blue. The light from one is 680 light years away, the light from the other 690 light years away. In the larger telescope, two more optical companions are added. \ No newline at end of file diff --git a/en/star/hr280.md b/en/star/hr280.md deleted file mode 100644 index 77ec96b4f..000000000 --- a/en/star/hr280.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Scl -constellation: Scl -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 08:46:13.324577 ---- - The brightest star, which is only 4.39 mag, gives a good indication of the constellation's prominence. Its probable distance is 780 light years. Just north of it lies the South Galactic Pole. \ No newline at end of file diff --git a/en/star/hr2878.md b/en/star/hr2878.md deleted file mode 100644 index 3dc19e4aa..000000000 --- a/en/star/hr2878.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: σ Pup -constellation: Pup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 12:01:17.289410 ---- -a nice binary star that can be resolved with a 5 cm telescope. The main orange component has a brightness of 3.3mag and its yellow companion at a distance of 22.3" reaches only 9.4mag. \ No newline at end of file diff --git a/en/star/hr2891.md b/en/star/hr2891.md deleted file mode 100644 index cd5370670..000000000 --- a/en/star/hr2891.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Kastor (α Gem) -constellation: Gem -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:13:09.872387 ---- -Although Pollux is slightly brighter, the Greek alpha letter is Kastor (the 23rd brightest star in the sky). It has a brightness of 1.5mag and is 51 light years from Earth. In addition, it is a known multiple system. The main component has a luminosity of 1.9mag and is 22 times brighter overall than the Sun, with the guide reaching 2.9mag. They orbit each other around a common centre of gravity in 445 years. The pair's angular separation has been quite small in recent years, reaching its minimum of 1.9" in 1970. Since then, it has gradually increased again, so that these blue components can be resolved with a small telescope. In 1985 their distance was 2.6" and by 2017 it had grown to 6". \ No newline at end of file diff --git a/en/star/hr2943.md b/en/star/hr2943.md deleted file mode 100644 index dc25a71b6..000000000 --- a/en/star/hr2943.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Procyon (α Cmi) -constellation: CMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:53:38.462160 ---- -means "before the dog" in Greek, because when viewed from most places in the northern hemisphere it rises slightly earlier than Sirius, the Dog Star. It is the eighth brightest star in the sky (0.5mag) and one of the closest, being 11.4 light years away. Among the bright stars, only Alpha Centauri and Sirius are closer. Procyon is easy to find, with the stars Sirius and Betelgeuse forming an equilateral triangle that arcs across the celestial equator and is visible from all latitudes. It is called the Winter Triangle, and its curious feature is that in the southern hemisphere it is best seen above the horizon during the height of the local summer. The procyon moves across the stellar background by the diameter of the Moon in 1,000 years, or 1.25" per year. \ No newline at end of file diff --git a/en/star/hr2990.md b/en/star/hr2990.md deleted file mode 100644 index c2173e20e..000000000 --- a/en/star/hr2990.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Pollux (β Gem) -constellation: Gem -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:12:33.226361 ---- -with a brightness of 1.14mag is the 17th brightest star in the sky. Its luminosity is 33 times that of the Sun, and its diameter is 9 times larger. Unlike Kastoria, Pollux is orange-red and has a spectral class of K0. Its striking hue can be seen with the naked eye. It is located at a distance of 34 light years. \ No newline at end of file diff --git a/en/star/hr310.md b/en/star/hr310.md deleted file mode 100644 index 78d086400..000000000 --- a/en/star/hr310.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ψ Psc -constellation: Psc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.320401 ---- diff --git a/en/star/hr3110.md b/en/star/hr3110.md deleted file mode 100644 index 148165896..000000000 --- a/en/star/hr3110.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 14 CMi -constellation: CMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 21:54:27.258638 ---- -the triple stars. The main star has a brightness of 5.4mag. At a distance of 76" is a 7th magnitude star and at a distance of 112" is a star with a brightness of 8mag. A good sorter or a telescope with a 5 cm diameter objective lens will suffice to resolve them. \ No newline at end of file diff --git a/en/star/hr3165.md b/en/star/hr3165.md deleted file mode 100644 index 43b7b1d71..000000000 --- a/en/star/hr3165.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Naos (ζ Puppis) -constellation: Pup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 12:00:37.016074 ---- -Since the Argo originally considered itself as a single constellation, the procedure for designating stars with Greek letters is the same for all its divided parts. Therefore, we find no alpha, beta, gamma or delta Puppis in Argo, the brightest star being only ζ Puppis, which reaches a brightness of 2.3mag. \ No newline at end of file diff --git a/en/star/hr3188.md b/en/star/hr3188.md deleted file mode 100644 index 8596aa58a..000000000 --- a/en/star/hr3188.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ζ Mon -constellation: Mon -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 10:12:17.085476 ---- -an optical binary star. The main component has a brightness of 5mag, its companion 8.5mag. It lies at a distance of 66.4". The other companion is at 32". We need binoculars with a 7cm diameter objective lens. \ No newline at end of file diff --git a/en/star/hr3207.md b/en/star/hr3207.md deleted file mode 100644 index 1131b5c5b..000000000 --- a/en/star/hr3207.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ Velorum -constellation: Vel -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-08 14:29:44.425945 ---- -a binocularly resolved binary whose main component, 2mag, is the brightest known Wolf-Rayet star, very warm and unstable, ejecting a lot of matter at an astonishing rate. Even in simple mass spectrographs one can see distinct emission in the blue region of the spectrum, lines of highly ionized atoms shining in the vast warm envelope illuminated by the star. γ Velorum is at an advanced stage of its evolution and shines about 3,800 times brighter than the Sun. But this won't be the case forever. After a few million years, it could explode as a supernova. It's 840 light years away. diff --git a/en/star/hr3208.md b/en/star/hr3208.md deleted file mode 100644 index 90cc0c0b7..000000000 --- a/en/star/hr3208.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Tegmin (ζ Cancri) -constellation: Cnc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 21:36:36.762520 ---- -triple constellation, the two most prominent components with 5.6mag and 6.2mag are 5.7" apart, which can be seen with a 5 cm telescope. Their mutual orbital period is about 1,100 years. The brighter star itself is a close binary - the companion of brightness about 6mag lies 0.8" apart. It can be resolved well with binoculars with a 300mm diameter lens. Its orbital period is 59.6 years; in 1991 its separation was only 0.5". \ No newline at end of file diff --git a/en/star/hr322.md b/en/star/hr322.md deleted file mode 100644 index de72faf99..000000000 --- a/en/star/hr322.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: β Phe -constellation: Phe -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.174206 ---- diff --git a/en/star/hr3223.md b/en/star/hr3223.md deleted file mode 100644 index 994389f7f..000000000 --- a/en/star/hr3223.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Vol -constellation: Vol -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-24 07:39:15.192924 ---- -a binary star made up of 4mag and 7mag components that can be resolved with a small telescope. Their separation is 6". \ No newline at end of file diff --git a/en/star/hr3248.md b/en/star/hr3248.md deleted file mode 100644 index fae3a677d..000000000 --- a/en/star/hr3248.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Cancri -constellation: Cnc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 21:38:18.707334 ---- -Mira Ceti is a variable star with magnitude variations from 6.1 to 11.8 with a period of 362 days. \ No newline at end of file diff --git a/en/star/hr3301.md b/en/star/hr3301.md deleted file mode 100644 index 4b038cf8b..000000000 --- a/en/star/hr3301.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: κ Vol -constellation: Vol -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-24 07:39:34.342895 ---- -a double star easily distinguishable even by a triad. The main component with a brightness of 5.4mag has a guide of 5.7mag at a distance of 65 arc seconds. At a distance of 37 arcseconds lies a 9th magnitude guide star. \ No newline at end of file diff --git a/en/star/hr3318.md b/en/star/hr3318.md deleted file mode 100644 index e36d5fb03..000000000 --- a/en/star/hr3318.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Cha -constellation: Cha -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-24 14:46:22.562828 ---- -the brightest star in the constellation. It has an apparent brightness of only 4.08mag. This white giant of spectral class F5 is 64 light-years away. \ No newline at end of file diff --git a/en/star/hr3340.md b/en/star/hr3340.md deleted file mode 100644 index 9a11f0761..000000000 --- a/en/star/hr3340.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: θ Cha -constellation: Cha -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-24 14:46:42.828673 ---- -an optical binary whose components appear close together in the sky, even from Earth, but are actually very far apart in space. The closer 4.3mag is 100 light years away, the fainter one is up to 1 000 light years away. \ No newline at end of file diff --git a/en/star/hr3347.md b/en/star/hr3347.md deleted file mode 100644 index 83b035c5d..000000000 --- a/en/star/hr3347.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Vol -constellation: Vol -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-24 07:38:34.340639 ---- -the brightest star in the constellation, a constant of apparent brightness 3.7mag. This orange giant lies at a distance of 108 light years. \ No newline at end of file diff --git a/en/star/hr338.md b/en/star/hr338.md deleted file mode 100644 index fc792df3e..000000000 --- a/en/star/hr338.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ζ Phe -constellation: Phe -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.654034 ---- diff --git a/en/star/hr34.md b/en/star/hr34.md deleted file mode 100644 index 2fc791f23..000000000 --- a/en/star/hr34.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: κ1 Scl -constellation: Scl -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 08:46:59.069386 ---- -a binary star of bright components 6.1mag and 6.2mag, but they lie quite close together - 1.4". Both are yellow in colour. \ No newline at end of file diff --git a/en/star/hr3433.md b/en/star/hr3433.md deleted file mode 100644 index 5e20315da..000000000 --- a/en/star/hr3433.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ζ Pyx -constellation: Pyx -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.131463 ---- diff --git a/en/star/hr3438.md b/en/star/hr3438.md deleted file mode 100644 index 8ad4a97cb..000000000 --- a/en/star/hr3438.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: β Pyx -constellation: Pyx -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.318235 ---- diff --git a/en/star/hr3468.md b/en/star/hr3468.md deleted file mode 100644 index 0f9802cf6..000000000 --- a/en/star/hr3468.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: α Pyx -constellation: Pyx -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.841117 ---- diff --git a/en/star/hr3475.md b/en/star/hr3475.md deleted file mode 100644 index 037888498..000000000 --- a/en/star/hr3475.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ι2 Cancri -constellation: Cnc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 21:34:36.092511 ---- - a triple star that even a 30 cm telescope can't distinguish. Under good viewing conditions, it is visible only as an elongated star, with a hint of a main yellow and a second blue component. \ No newline at end of file diff --git a/en/star/hr3482.md b/en/star/hr3482.md deleted file mode 100644 index d8e840d97..000000000 --- a/en/star/hr3482.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Hya -constellation: Hya -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:41:42.323586 ---- -the main component with a brightness of 3.8mag has a guide of 6.9mag at a distance of 2.8". To resolve this double star, we need a telescope with a lens diameter of at least 8 cm. The components orbit each other in 870 years and lie at a distance of 129ly. \ No newline at end of file diff --git a/en/star/hr3485.md b/en/star/hr3485.md deleted file mode 100644 index 2fc0a6d40..000000000 --- a/en/star/hr3485.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Vel -constellation: Vel -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-08 14:33:10.672253 ---- -the brightest star in the constellation with an inverted brightness of 2mag. Together with the stars κ Vel and ε and ι Car of the Carina, they form the so-called False Cross, which novice observers often confuse with the true Southern Cross. Unlike the latter, however, it is slightly larger, more symmetrical and less bright, and its arm does not point to the region of the south celestial pole. \ No newline at end of file diff --git a/en/star/hr3541.md b/en/star/hr3541.md deleted file mode 100644 index 5d05ff578..000000000 --- a/en/star/hr3541.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: X Cancri -constellation: Cnc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 21:35:53.641951 ---- -A variable star with a striking red hue, it changes magnitude from 5.6 to 7.5mag in about 195 days, suitable for trinary tracking. It is located near the star δ Cancri. \ No newline at end of file diff --git a/en/star/hr3572.md b/en/star/hr3572.md deleted file mode 100644 index fffd9276d..000000000 --- a/en/star/hr3572.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Acubens (α Cancri) -constellation: Cnc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 21:35:21.499015 ---- -a binary star only distinguishable with a larger telescope. The guide lies 11.3" from the main component (4.25mag), but is about 1,000 times fainter and has a brightness of only 11.8mag in the sky. The system lies at a distance of 164 light years. \ No newline at end of file diff --git a/en/star/hr361.md b/en/star/hr361.md deleted file mode 100644 index c052d8563..000000000 --- a/en/star/hr361.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ζ Psc -constellation: Psc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.405787 ---- diff --git a/en/star/hr3628.md b/en/star/hr3628.md deleted file mode 100644 index b100f5736..000000000 --- a/en/star/hr3628.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: κ Pyx -constellation: Pyx -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.963739 ---- diff --git a/en/star/hr3644.md b/en/star/hr3644.md deleted file mode 100644 index 8504c5191..000000000 --- a/en/star/hr3644.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ε Pyx -constellation: Pyx -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.691232 ---- diff --git a/en/star/hr3690.md b/en/star/hr3690.md deleted file mode 100644 index 7943569bf..000000000 --- a/en/star/hr3690.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 38 Lyn -constellation: Lyn -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:51:20.365490 ---- -a double star approximately on the boundary with the neighbouring constellation of the Little Lion. The main white component reaches a brightness of 3.9mag, the rusty guide 6.6mag. They are 2.7" apart and their distance from Earth is about 117 light years. The main star has about 32 times the luminosity of the Sun. At a distance of about 88" from this star we see another guide star of stellar magnitude 11mag, but it only projects into this region by chance. It is advisable to use at least 100x magnification. \ No newline at end of file diff --git a/en/star/hr3748.md b/en/star/hr3748.md deleted file mode 100644 index a928cc9b3..000000000 --- a/en/star/hr3748.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alfard (α Hya) -constellation: Hya -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:41:12.826387 ---- -the brightest star in the constellation, lies at the conjunction of the stars Kastor - Pollux of Gemini. Its remarkable orange colouring can certainly be seen with the naked eye, and it belongs to the spectral class K3. This giant reaches 2mag and is located in a relatively star-poor region. That is why its translated name from Arabic means "Solitary Star". Tycho de Brahe, however, called it Cor Hydraul - "Heart of the Hydra". It lies at a distance of 177 light years and is 780 times more luminous than the Sun. \ No newline at end of file diff --git a/en/star/hr377.md b/en/star/hr377.md deleted file mode 100644 index 01cec7108..000000000 --- a/en/star/hr377.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: κ Tuc -constellation: Tuc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-24 07:42:49.740613 ---- -a binary star composed of 5 and 8 mag stars that can be resolved with a small telescope. \ No newline at end of file diff --git a/en/star/hr3787.md b/en/star/hr3787.md deleted file mode 100644 index 2b8d255c4..000000000 --- a/en/star/hr3787.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: τ1 Hya -constellation: Hya -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:43:18.915658 ---- -The 4.8mag and 8mag components lie 65" apart. This is an optical binary star, for which even binoculars are sufficient to resolve. \ No newline at end of file diff --git a/en/star/hr3789.md b/en/star/hr3789.md deleted file mode 100644 index f8145e675..000000000 --- a/en/star/hr3789.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ζ Antliae -constellation: Ant -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:10:33.332476 ---- -a multiple star that the binocular splits into two broad optical components of sixth magnitude. Moreover, with a small telescope we find that the brighter of the two is itself a binary star - the yellow 7.1-mag companion is eight arc seconds away. \ No newline at end of file diff --git a/en/star/hr3798.md b/en/star/hr3798.md deleted file mode 100644 index 8c1d60b1c..000000000 --- a/en/star/hr3798.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: S Antliae -constellation: Ant -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:11:06.401354 ---- -discovered in 1888, is an eclipsing variable star with a brightness change of 0.5mag in exactly 7 hours and 47 minutes. At the time of its discovery, it was known as the variable star with the shortest period of brightness change. It is included in the group of stars known as the W URSA Majoris type, a system where two dwarf stars orbit each other in close contact, causing their positions to constantly change from our point of view. \ No newline at end of file diff --git a/en/star/hr3816.md b/en/star/hr3816.md deleted file mode 100644 index 1bc500563..000000000 --- a/en/star/hr3816.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Carinae -constellation: Car -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:00:28.790151 ---- -a variable star of the type Mira Ceti with a magnitude range from 3.9 to 10.5 and a period of 309 days. \ No newline at end of file diff --git a/en/star/hr3882.md b/en/star/hr3882.md deleted file mode 100644 index 7a979b054..000000000 --- a/en/star/hr3882.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Leonis -constellation: Leo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:41:28.107370 ---- -a variable star of the type Mira Ceti in the western part of the constellation, near Regulus, 372 light years away. This red giant varies in brightness from 4.4mag to 11.3mag with a long period of 312.43 days. It is therefore one of the brightest long-period variable stars. At the time of maximum, we can notice its distinct, deep red hue, which contrasts nicely with the white star 19 Leonis, 8' to the south. \ No newline at end of file diff --git a/en/star/hr3981.md b/en/star/hr3981.md deleted file mode 100644 index 0c68c9fc0..000000000 --- a/en/star/hr3981.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Sex -constellation: Sex -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 12:02:59.687941 ---- -the brightest star in the constellation has an apparent brightness of 4.5mag. It lies almost exactly on the celestial equator. It is 270 light years away. \ No newline at end of file diff --git a/en/star/hr3982.md b/en/star/hr3982.md deleted file mode 100644 index 3cf621fa0..000000000 --- a/en/star/hr3982.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Regulus (α Leonis) -constellation: Leo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:26:28.595677 ---- -the brightest star in the constellation. The 9-fold elongation of the front wheels of the Big Dipper will lead us to it in a southerly direction. Together with the stars Arcturus of Shepherd and Spica of Virgo, it forms a kind of spring triangle. The name comes from Latin and means "little king"; indeed, in ancient Babylon it always represented the star of the ruler. Sometimes we can also meet the name Cor Leonis - "heart of the lion". Regulus is also one of the four guardians of the sky, or even royal stars - they were the stars that marked the summer solstice point (Regulus), the spring point (Aldebaran), the winter solstice (Fomalhaut) and the autumn point (Antares) in the Persian Empire. These divided the sun's orbit - the ecliptic - and thus the year into four seasons. It is one of the few bright stars that lies near the ecliptic, exactly 1.5 degrees. That's why it's often occulted by the moon and sometimes a planet. \ No newline at end of file diff --git a/en/star/hr3989.md b/en/star/hr3989.md deleted file mode 100644 index 8e79dc5bd..000000000 --- a/en/star/hr3989.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 17 a 18 Sex -constellation: Sex -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 12:03:40.123314 ---- -a broad pair of unrelated stars that can be identified with the naked eye if the observer has good eyesight. They are easily separated by a trier. They have brightnesses of 5.9 and 5.6mag. The components are 530 and 470 light years apart. \ No newline at end of file diff --git a/en/star/hr4031.md b/en/star/hr4031.md deleted file mode 100644 index 1013d97a8..000000000 --- a/en/star/hr4031.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ζ Leonis -constellation: Leo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:39:06.511874 ---- -a wide triple star, composed of stars that have no relationship to each other. ζ Leonis has a brightness of 3.4 mag. The binocular shows the star 35 Leonis to the north of it and 39 Leonis further south. Both reach 6 mag. \ No newline at end of file diff --git a/en/star/hr4057.md b/en/star/hr4057.md deleted file mode 100644 index ab275e5f2..000000000 --- a/en/star/hr4057.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Algieba (γ Leonis) -constellation: Leo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:38:32.037612 ---- -"Lion's forehead", a corruption of the Arabic word Al Jabha. Actually a magnificent binary star lying 8 degrees SSE of Regulus, with yellow-orange components of 2.2mag (lum. 90 Suns) and 3.5mag (lum. 30 Suns) at a distance of 4.4", in contrast to each other they can be seen as far as green. Their mutual orbital period is estimated at 619 years. As recently as 1782, when this attractive double star was first discovered by William Herschel, the arc distance of its components was less than 2". Since then, the distance has increased significantly, reaching nearly 4.4" by the end of the 20th century. \ No newline at end of file diff --git a/en/star/hr4100.md b/en/star/hr4100.md deleted file mode 100644 index b2f144fd3..000000000 --- a/en/star/hr4100.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β LMi -constellation: LMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:43:50.982559 ---- -the only star in the constellation to be assigned a Greek letter. This tight binary, which looks like a bright 4.2mag point when viewed with the naked eye, will only show its 6.1mag companion in a large telescope and during good viewing conditions. It is located at an angular distance of only a few tenths of a second. The components have an orbital period of 37 years and a distance of 145 light years. \ No newline at end of file diff --git a/en/star/hr4104.md b/en/star/hr4104.md deleted file mode 100644 index 431bb7971..000000000 --- a/en/star/hr4104.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Antliae -constellation: Ant -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:09:47.567753 ---- -the brightest star in the constellation is 4.25mag, in many constellations it would go unnoticed. In the binocular, we can see its orange to red hue. Its spectral class is K4, so it's a cooler star than our Sun. Its brightness probably fluctuates slightly and it's 370 light years away. \ No newline at end of file diff --git a/en/star/hr4163.md b/en/star/hr4163.md deleted file mode 100644 index 8ac8a94f7..000000000 --- a/en/star/hr4163.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: U Hya -constellation: Hya -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:42:20.781557 ---- -one of the brightest and most unusual carbon stars, whose red colour can be seen even in the smallest binocular. This is due to the abundance of carbon molecules in its atmosphere that absorb blue light. U Hya is observed 4 degrees northwest of ν Hydra and is one of the irregular variable stars whose magnitude varies with some regularity from 4.7mag to 6.2mag over a period of about 450 days. It is about 680 light years away. \ No newline at end of file diff --git a/en/star/hr4193.md b/en/star/hr4193.md deleted file mode 100644 index 00cf220fa..000000000 --- a/en/star/hr4193.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 35 Sex -constellation: Sex -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 12:03:17.273799 ---- -a nice pair of orange 6.3mag and yellow-orange 7.4mag components, which are easily distinguishable even in a small amateur telescope. Their separation is 6.8". \ No newline at end of file diff --git a/en/star/hr4210.md b/en/star/hr4210.md deleted file mode 100644 index 5b6b5c8d4..000000000 --- a/en/star/hr4210.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: η Carinae -constellation: Car -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:01:08.442163 ---- -an unusual variable star, massive and unstable, which may explode as a supernova in the future. In 1677, Edmund Halley recorded that the star had brightened to 4th magnitude. In 1730 it reached second magnitude, by 1827 it had brightened to first magnitude and during April 1843 it temporarily became the second brightest star in the sky after the spread, with a brightness of -0.8mag! In the following years its brightness decreased and from 1868 it ceased to be visible sometimes without a trier, as its brightness was around 6th magnitude. In the infrared, however, it is still the brightest source in the sky. \ No newline at end of file diff --git a/en/star/hr4216.md b/en/star/hr4216.md deleted file mode 100644 index 0e85337f9..000000000 --- a/en/star/hr4216.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: μ Vel -constellation: Vel -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-08 14:33:46.889995 ---- -a physical binary whose components orbit in 116 years. Their luminosities are 2.7mag and 6.4mag, with a separation of about 2.3" at present. \ No newline at end of file diff --git a/en/star/hr423.md b/en/star/hr423.md deleted file mode 100644 index 112e0ad68..000000000 --- a/en/star/hr423.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Scl -constellation: Scl -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 09:52:32.991701 ---- -a variable red giant whose brightness varies on an approximately annual cycle from 6 to 8mag. \ No newline at end of file diff --git a/en/star/hr4234.md b/en/star/hr4234.md deleted file mode 100644 index 73e714a68..000000000 --- a/en/star/hr4234.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Cha -constellation: Cha -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-24 14:48:32.713979 ---- -a wide binary star whose 4.4mag and 5.5mag brightness components are 7' apart, so we can distinguish them with the naked eye. In the binocular we can see their different white and orange hues. It is an optical binary: the brighter component is 364 light years away, the fainter one is 10 light years closer. However, the brighter component is actually a very close physical binary, which can only be resolved with a large telescope. \ No newline at end of file diff --git a/en/star/hr424.md b/en/star/hr424.md deleted file mode 100644 index 418ad0f25..000000000 --- a/en/star/hr424.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Polaris (α UMi) -constellation: UMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:21:55.345307 ---- -On the seas, in the desert and in the wilderness, it was in ancient times, before the invention of the compass, the only indicator of north. It is easily found by plotting the distance of the stars Merak and Dubhe, which form the back wheels of the Big Dipper, 4 times in the direction of the line of the line, and we reach Polaris, which is at the end of the drawbar of the Little Dipper. \ No newline at end of file diff --git a/en/star/hr4259.md b/en/star/hr4259.md deleted file mode 100644 index 2e412d5fe..000000000 --- a/en/star/hr4259.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 54 Leonis -constellation: Leo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:40:18.511668 ---- -a binary star lying just on the boundary with the constellation of the Little Lion. These two partners have brightnesses of 4.5mag and 6.3mag. The two stars are 6.5" apart, so they should already be distinguishable with a telescope with a lens diameter of at least 5 cm. The system is 330 light years from Earth. In 10-15 cm telescopes and 100x magnification, it is an unequally bright, colorful binary. The main component appears yellow-white, the guide is bluish to greenish. \ No newline at end of file diff --git a/en/star/hr4287.md b/en/star/hr4287.md deleted file mode 100644 index 0058aa004..000000000 --- a/en/star/hr4287.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alkes (α Crt) -constellation: Crt -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 17:21:15.641285 ---- - The Arabic name of the main star means "flat bowl". Its brightness is only 4.2mag. It's a yellow giant that radiates 66 times more than our sun. It's 141 light years away from us. \ No newline at end of file diff --git a/en/star/hr4375.md b/en/star/hr4375.md deleted file mode 100644 index c0f305ee7..000000000 --- a/en/star/hr4375.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ξ UMa -constellation: UMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-03 20:44:01.227282 ---- -the first binary star where the orbit of the components was calculated, and it was 60 years. The French astronomer Felix Savary succeeded in 1828. It is made up of golden components with a brightness of 4.3mag and 4.8mag, 3 billion kilometres apart. Around 1970 they were 3" apart and could be easily distinguished with small telescopes. Then their separation decreased, reaching a minimum of 0.8" in 1992. Today, the value is around 2", so a telescope with an 8 cm lens diameter is sufficient to distinguish them. \ No newline at end of file diff --git a/en/star/hr4382.md b/en/star/hr4382.md deleted file mode 100644 index 42fefe5b1..000000000 --- a/en/star/hr4382.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Crt -constellation: Crt -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 17:20:54.603334 ---- -the brightest star in the constellation reaches an apparent brightness of 3.82mag. It is about 163 light years from Earth and 171 times more luminous than our Sun \ No newline at end of file diff --git a/en/star/hr4399.md b/en/star/hr4399.md deleted file mode 100644 index 88e7ef7fb..000000000 --- a/en/star/hr4399.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ι Leonis -constellation: Leo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:39:36.413071 ---- -a remarkable double star. The two components with brightnesses of 4.1mag and 7.0mag orbit each other in about 180 years. In 1985, they were 1.3" apart, but they begin to drift apart, reaching 1.7" by the year 2000, making the binary resolvable in at least a 10 cm telescope. \ No newline at end of file diff --git a/en/star/hr4405.md b/en/star/hr4405.md deleted file mode 100644 index f186d03b0..000000000 --- a/en/star/hr4405.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ Crt -constellation: Crt -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 17:21:50.740583 ---- -the 4.1mag main component has a 9.6mag guide at a distance of 5.2", which we can find with binoculars with a lens diameter of about 10 cm. The brighter component is white, the guide is blue. Their light has been flying towards us for 85 years. \ No newline at end of file diff --git a/en/star/hr4418.md b/en/star/hr4418.md deleted file mode 100644 index b86d360be..000000000 --- a/en/star/hr4418.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: τ Leonis -constellation: Leo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:40:53.911552 ---- -a double star, easily distinguishable with a simple trier. The main star has a brightness of 5.4mag and its companion 7.0mag. The angular separation of the two partners is 90". \ No newline at end of file diff --git a/en/star/hr4534.md b/en/star/hr4534.md deleted file mode 100644 index 5f571a75c..000000000 --- a/en/star/hr4534.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Denebola (β Leonis) -constellation: Leo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:26:58.340184 ---- -has a luminosity of 2.2mag and its distance from Earth is 36 light years. It's 15 times brighter than the sun. At a distance of almost 19 arc minutes, we find a yellowish star with a brightness of 6mag, which we can already see through a theatre peephole. \ No newline at end of file diff --git a/en/star/hr4602.md b/en/star/hr4602.md deleted file mode 100644 index 76fa56712..000000000 --- a/en/star/hr4602.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 2 Com -constellation: Com -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:41:30.522766 ---- -nice pair of two yellow components (5,9mag and 7,4mag). A telescope with a lens diameter over 10 cm can resolve this double star at 3.7" at higher magnification. \ No newline at end of file diff --git a/en/star/hr462.md b/en/star/hr462.md deleted file mode 100644 index 34e635c83..000000000 --- a/en/star/hr462.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: τ Scl -constellation: Scl -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 09:52:15.850789 ---- -a close pair (2.2") of bright yellow stars 6mag and 7.1mag. \ No newline at end of file diff --git a/en/star/hr472.md b/en/star/hr472.md deleted file mode 100644 index ff81b1e2d..000000000 --- a/en/star/hr472.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Achernar (α Eri) -constellation: Eri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.163264 ---- diff --git a/en/star/hr4730.md b/en/star/hr4730.md deleted file mode 100644 index cbc590188..000000000 --- a/en/star/hr4730.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Acrux (α Cru) -constellation: Cru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-26 20:39:40.301461 ---- -the constellation's brightest star at 1.1mag and the 13th brightest star in the sky. In binoculars it can be resolved into two brilliant blue-white components 4.4" apart. They have a brightness of 0.8mag and 2.1mag, and a 60mm telescope is sufficient to separate them. The system lies at a distance of 370 light years. A third unrelated 5mag component is found 90" away. \ No newline at end of file diff --git a/en/star/hr4757.md b/en/star/hr4757.md deleted file mode 100644 index 0bbc99f60..000000000 --- a/en/star/hr4757.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Algorab (δ Crv) -constellation: Crv -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 17:03:58.226269 ---- - Through a telescope with a lens diameter of at least 8 cm, we see a faint pale blue companion of 9th magnitude at a distance of 24.2" from the bright white component of the third magnitude. This system is 88 light years away. \ No newline at end of file diff --git a/en/star/hr4763.md b/en/star/hr4763.md deleted file mode 100644 index 4b42dc241..000000000 --- a/en/star/hr4763.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Gacrux (γ Cru) -constellation: Cru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-26 20:40:25.962120 ---- -red giant (1.6mag), which contrasts nicely with the three other hot blue-white stars of the cross. In fact, it is an optical binary, a companion of 6.5mag brightness found in the trinary at a distance of 2'. The red giant is 88 light years away, the companion is three times farther away. \ No newline at end of file diff --git a/en/star/hr4792.md b/en/star/hr4792.md deleted file mode 100644 index c4aa29184..000000000 --- a/en/star/hr4792.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 24 Com -constellation: Com -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:39:55.704352 ---- -double star, components 5.2mag and 6.7mag at 20.3". In at least a 10 cm telescope, nice color contrast of the main yellow-orange and fainter blue stars, similar to Albireo of the Swan. Otherwise we can distinguish them with a better binocular. \ No newline at end of file diff --git a/en/star/hr4798.md b/en/star/hr4798.md deleted file mode 100644 index b8361562d..000000000 --- a/en/star/hr4798.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: α Mus -constellation: Mus -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.733405 ---- diff --git a/en/star/hr4808.md b/en/star/hr4808.md deleted file mode 100644 index 396aee7a6..000000000 --- a/en/star/hr4808.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Virginis -constellation: Vir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-04 20:33:09.212383 ---- -a variable star of the type Mira Ceti, with a magnitude change from 6.0 to 12.1 over 146 days. It is believed to be a red M-class star. \ No newline at end of file diff --git a/en/star/hr4825.md b/en/star/hr4825.md deleted file mode 100644 index 35a82b526..000000000 --- a/en/star/hr4825.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Porrima (γ Virginis) -constellation: Vir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-04 20:29:33.840350 ---- - one of the most beautiful double stars in the sky, both yellow-white components have almost the same brightness of 3.5mag and at the same distance of 3" they can be observed with a 6 cm telescope. Their orbital period around their common centre of gravity is 171.85 years. They reached their greatest separation in 1920 - 6.2", so they could be seen in a 5 cm telescope. Meanwhile, their distance from each other is rapidly decreasing. In 1985 the value reached 3.5", in 2000 only 1.8". Therefore, nowadays we need at least 200 mm to distinguish two point stars in good seeing conditions. In 2007 the separation will be even smaller, reaching only 0.3", and therefore we will need a much larger telescope to resolve them. The system is 32 light years away. Five arc degrees to the north lies the brightest quasar - a 13th magnitude, designated 3 C 273, approximately 3 billion light years away. \ No newline at end of file diff --git a/en/star/hr4844.md b/en/star/hr4844.md deleted file mode 100644 index 819f4a23d..000000000 --- a/en/star/hr4844.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: β Mus -constellation: Mus -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.618562 ---- diff --git a/en/star/hr4846.md b/en/star/hr4846.md deleted file mode 100644 index e3bd122e6..000000000 --- a/en/star/hr4846.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Y CVn (E-B 364) -constellation: CVn -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 14:39:46.323124 ---- -"La Superba" is the name given to this distinctive red star by Italian astronomer Angelo Secchi in the 19th century. It is a variable star that changes its brightness from 4.8mag to 6.4mag over a period of 157 days. The striking red hue can be seen quite easily in 50-60 mm telescopes. The unusual, deep red colour of this and similar stars is due to carbon molecules (which are abundant in the atmosphere) absorbing the star's blue light. \ No newline at end of file diff --git a/en/star/hr4853.md b/en/star/hr4853.md deleted file mode 100644 index 2cee02f69..000000000 --- a/en/star/hr4853.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Cru -constellation: Cru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-26 20:39:14.125835 ---- -a pale blue giant 350 light years away. With a brightness of 1.3 mag, it ranks among the 20 brightest stars in the sky. Its pulsation changes its size five times a day, and its magnitude changes by less than a tenth, but this is not enough to notice with the naked eye. \ No newline at end of file diff --git a/en/star/hr4898.md b/en/star/hr4898.md deleted file mode 100644 index 99dde3b04..000000000 --- a/en/star/hr4898.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: μ Cru -constellation: Cru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-26 20:40:54.497534 ---- -a wide optical binary star that a small telescope or powerful binocular shows as two stars with brightnesses of 4.1 and 5.1 mag. The fainter star rotates rapidly around the primary star spewing jets of gas, causing occasional small changes in brightness. \ No newline at end of file diff --git a/en/star/hr4905.md b/en/star/hr4905.md deleted file mode 100644 index 789b5b15e..000000000 --- a/en/star/hr4905.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alioth (ε UMa) -constellation: UMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-03 20:42:40.164970 ---- -the brightest star in the constellation. It is a short-period variable star and a binary whose components have a mutual orbital period of 4.15 years, but this can only be discerned by spectroscopic methods. The variation in its brightness over a period of 5.09 days is only 0.1mag and therefore not perceptible to the naked eye. The star belongs to the type of stars α2 Canum Venaticorum, which also show magnetic field fluctuations. \ No newline at end of file diff --git a/en/star/hr4915.md b/en/star/hr4915.md deleted file mode 100644 index 59cae11b9..000000000 --- a/en/star/hr4915.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Cor Caroli (α CVn) -constellation: CVn -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 14:38:52.946497 ---- -"The Heart of Charles", the brightest star in the constellation. Edmund Halley so named the star at the suggestion of the court physician and physicist Sir Charles Scarborough, who claimed at the English court that the star shone exceptionally brightly on 29 May 1660, when King Charles II of England, founder of the Greenwich Observatory, returned to London. Another story says that it was the heart of King Charles I, executed on the orders of Oliver Cromwell in the mid-17th century, that made its way into the sky. \ No newline at end of file diff --git a/en/star/hr4952.md b/en/star/hr4952.md deleted file mode 100644 index 87109a557..000000000 --- a/en/star/hr4952.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: θ Mus -constellation: Mus -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.298697 ---- diff --git a/en/star/hr4963.md b/en/star/hr4963.md deleted file mode 100644 index 44ad8743b..000000000 --- a/en/star/hr4963.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: θ Virginis -constellation: Vir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-04 20:30:35.689638 ---- -a remarkable triple star located 200 light years away. The two brighter components are 7.2" apart and have brightnesses of 4.4mag and 9.4mag. To resolve them, we need a telescope with a lens diameter of 6 to 8 cm. In a good 100 instrument, a third guide of 10.4mag will also show up at a distance of 69.6" from the main white star (the second component appears dull yellow). \ No newline at end of file diff --git a/en/star/hr4968.md b/en/star/hr4968.md deleted file mode 100644 index 64159d4ea..000000000 --- a/en/star/hr4968.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Diadem (α Com) -constellation: Com -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:40:59.560502 ---- -a star that appears to the naked eye to be a 4.3-mag point. In fact, it is a double star, consisting of two components of 5.1mag brightness, but we cannot distinguish them with a small telescope. They orbit each other in 25.85 years. \ No newline at end of file diff --git a/en/star/hr4990.md b/en/star/hr4990.md deleted file mode 100644 index 38433a104..000000000 --- a/en/star/hr4990.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 54 Virginis -constellation: Vir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-04 20:32:44.353835 ---- -attractive pair of yellow (6.8mag) and white stars (7.3mag) at a distance of 5.4" even in small telescopes at 100x magnification. \ No newline at end of file diff --git a/en/star/hr5054.md b/en/star/hr5054.md deleted file mode 100644 index b695bc7bf..000000000 --- a/en/star/hr5054.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Mizar a Alcor (ζ a 80 UMa) -constellation: UMa -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-03 20:43:24.035809 ---- -The most famous double star, which the Arabs used to refer to as "the guide" or "the tester of the sharpness of sight". The mutual distance of the two stars is 12', so that the healthy eye can distinguish them almost always without difficulty. They make a nice pair in binocular as well. \ No newline at end of file diff --git a/en/star/hr5056.md b/en/star/hr5056.md deleted file mode 100644 index c26c5116a..000000000 --- a/en/star/hr5056.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Spika (α Virginis) -constellation: Vir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-04 20:26:46.816769 ---- -the brightest star in the constellation, reaching 1st magnitude. This pure white, bright star can be used for orientation in the spring sky, because together with the stars Regulus in Leo and Arcturus in Arcturus, it forms the so-called spring triangle, a kind of analogue of the better known summer triangle. It is located at the elongated junction of the upper right and lower left wheels of the Big Dipper. It is about 250 light years away and 2,800 times the luminosity of the Sun. It is a very close spectroscopic binary (eclipsing variable star) with a period of 4.014 days. During this period, it undergoes periodic slight partial eclipses of about a tenth of its brightness, which are not visually noticeable. In addition, the main star of this pair shows a faint pulsation with a period of 0.174 days. Spica has a surface temperature of nearly 20,000 ˚C, shining with a power of more than a thousand Suns. \ No newline at end of file diff --git a/en/star/hr509.md b/en/star/hr509.md deleted file mode 100644 index e17ccb1e6..000000000 --- a/en/star/hr509.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: τ Cet -constellation: Cet -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 18:19:09.780381 ---- -its slow rotation points to the possible existence of a planetary system and thus to the possibility of the formation and existence of life in this yellow dwarf star similar to the Sun (in terms of temperature and luminous power). It would be one of our closest planetary systems, 11.85 ly from Earth. That's why it was chosen for the Ozma project, which aims to make contact with possible nearby civilizations on radio waves. Along with the epsilon star Eridani, it was also selected for the original SETI (Search for Extra.Terrestrial Intelligence) research project. \ No newline at end of file diff --git a/en/star/hr5127.md b/en/star/hr5127.md deleted file mode 100644 index f82f6519c..000000000 --- a/en/star/hr5127.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 25 Canum Venaticorum -constellation: CVn -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 14:40:41.129450 ---- - a binary star that splits into two yellow components of 5mag and 6.9mag in a 15 cm telescope. Their separation is 1.8". \ No newline at end of file diff --git a/en/star/hr514.md b/en/star/hr514.md deleted file mode 100644 index 64a0587f9..000000000 --- a/en/star/hr514.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Scl -constellation: Scl -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 08:46:36.853236 ---- -a physical binary star with an orbital period of 1 200 years, whose components have a brightness of 5.4mag and 8.6mag and are located 4.7" apart. We can resolve them with a 100 mm telescope. Both are yellow in colour and 92 light years away. \ No newline at end of file diff --git a/en/star/hr5159.md b/en/star/hr5159.md deleted file mode 100644 index 5fdae059b..000000000 --- a/en/star/hr5159.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 84 Virginis -constellation: Vir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-04 20:31:52.697888 ---- -A binary star consisting of a close pair of a bright orange (5.5mag) and a dull yellow component (7.9mag) at a distance of 2.9". A telescope with a lens diameter of about 100 mm is recommended for resolution. \ No newline at end of file diff --git a/en/star/hr5210.md b/en/star/hr5210.md deleted file mode 100644 index 6b035cb79..000000000 --- a/en/star/hr5210.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 3 Cen -constellation: Cen -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:21:13.923589 ---- -a remarkable pair of unequally bright pale blue stars of 4.5mag and 6mag, lying 7.9" apart. \ No newline at end of file diff --git a/en/star/hr5221.md b/en/star/hr5221.md deleted file mode 100644 index 79af15014..000000000 --- a/en/star/hr5221.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 4 Cen -constellation: Cen -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:23:03.129608 ---- -an attractive double star consisting of a pale blue 4.7mag and a grey-white 8.4mag component that lies 14.9" away. \ No newline at end of file diff --git a/en/star/hr5261.md b/en/star/hr5261.md deleted file mode 100644 index b38e382b8..000000000 --- a/en/star/hr5261.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: θ Aps -constellation: Aps -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:13:40.465614 ---- -a variable, distinct red star, at the limit of visibility to the naked eye during the peak. Its brightness varies between 6.4mag and 8mag with a period of just over 100 days. \ No newline at end of file diff --git a/en/star/hr5267.md b/en/star/hr5267.md deleted file mode 100644 index 4b97199eb..000000000 --- a/en/star/hr5267.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Hadar (β Centauri) -constellation: Cen -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:19:52.282965 ---- -or also Agena. With a magnitude of 0.9, it is the 10th brightest star in the sky. Together with the star Toliman, from which it lies only four and a half degrees, it forms a good landmark for identifying the Southern Cross, thus preventing confusion with the so-called False Cross, which is formed by the stars of the Ship's Keel and Sail. Although, unlike Toliman, this blue-white giant is fainter in the sky, it lies about 100 times farther away. Its absolute magnitude is -5.5. So if it were located where Toliman is, it would be about a -10th magnitude star! \ No newline at end of file diff --git a/en/star/hr5291.md b/en/star/hr5291.md deleted file mode 100644 index e1f0ffe4c..000000000 --- a/en/star/hr5291.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Thuban (α Dra) -constellation: Dra -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:18:20.644712 ---- -once the brightest star in the constellation, now only 3.6 mag. 4,800 years ago, in the time of ancient Egypt, it marked the north celestial pole, just 10 arc minutes away. However, it has since shifted towards Polaris as a result of the precession of the Earth's axis, and Thuban is now over 25 degrees from it. Thuban belongs to spectral class AO and lies midway between Mizar and Kochab. It is 215 light years away and 135 times brighter than the Sun. \ No newline at end of file diff --git a/en/star/hr5326.md b/en/star/hr5326.md deleted file mode 100644 index 9c3377202..000000000 --- a/en/star/hr5326.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Cen -constellation: Cen -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:23:49.829725 ---- -a Mira-type variable star, lies between α and β Centauri. Its brightness varies from 5.3mag to 11.8mag over 546 days. \ No newline at end of file diff --git a/en/star/hr5340.md b/en/star/hr5340.md deleted file mode 100644 index 7ce7bc621..000000000 --- a/en/star/hr5340.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Arcturus (α Bootis) -constellation: Boo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 18:12:20.869326 ---- -The "Guardian Bear" is the brightest star in the northern sky and the fourth brightest (0.0mag) after Sirius, Canopus and Alpha Centauri. It is targeted by the fourfold elongated downward conjunction of the stars of the Big Dipper's axis. Arcturus is the nearest orange giant, 35 light-years away and about 30 million km across, and is 20 times larger than the Sun, but exceeds it by up to 100 times in luminosity. \ No newline at end of file diff --git a/en/star/hr5409.md b/en/star/hr5409.md deleted file mode 100644 index f8a8dba5b..000000000 --- a/en/star/hr5409.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: φ Virginis -constellation: Vir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-04 20:31:24.578882 ---- - a triple constellation consisting of two stars (yellow and orange) with brightnesses of 4.8mag and 9.3mag, 4.8" apart, and a third bluish component of 12.4mag at a distance of 93". \ No newline at end of file diff --git a/en/star/hr544.md b/en/star/hr544.md deleted file mode 100644 index ec68710ce..000000000 --- a/en/star/hr544.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Mettalah (α Trianguli) -constellation: Tri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 14:52:06.771442 ---- - Latin "Caput Triangulo" - the apex of a triangle. Its brightness is 3.6mag and it is 63 light years away. It has two faint guides of 12mag and 12.9mag at angular distances of 222" and 83". \ No newline at end of file diff --git a/en/star/hr5459.md b/en/star/hr5459.md deleted file mode 100644 index a85dda6ed..000000000 --- a/en/star/hr5459.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Toliman (α Centauri) -constellation: Cen -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:19:28.724657 ---- -is the brightest star in the constellation and the third brightest star in the sky after Sirius and Canopus. However, it lies quite far to the south, and from 25 degrees north latitude it is visible only just above the horizon during the culmination. At a distance of 4.36 light years, it is our closest star visible to the naked eye. In reality, however, it is made up of two yellow components with brightnesses of 0.1mag and 1.3mag, which are usually easy to distinguish with a small telescope - at the turn of the millennium their separation reached 14.1". By 2035, that distance will shrink to just 2 arcseconds. Their mutual orbital period around their common centre of gravity is 80 years. The α Centauri system is our closest star system ever. However, our nearest star is actually a red dwarf of 10.7mag brightness called Proxima Centauri, which is also physically related to this system. \ No newline at end of file diff --git a/en/star/hr546.md b/en/star/hr546.md deleted file mode 100644 index abcefc832..000000000 --- a/en/star/hr546.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Mesarthim (γ Arietis) -constellation: Ari -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:31:41.747353 ---- -a lovely double star, consisting of blue-white components 4.7mag and 4.8mag at a distance of 7.8", which can be resolved with a 5 cm telescope. Mesarthim appears to the naked eye as a 3.9mag star. Historically, it is interesting because it was one of the first double stars discovered with a telescope, registered by the English naturalist Robert Hooke in 1664 on the occasion of a comet sighting. It is 204 light years away. \ No newline at end of file diff --git a/en/star/hr5463.md b/en/star/hr5463.md deleted file mode 100644 index ba79b5697..000000000 --- a/en/star/hr5463.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Cir -constellation: Cir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-24 19:47:09.072091 ---- -the brightest star in the constellation has an apparent brightness of 3.4mag. At a distance of 15.7" lies the 8.6mag companion, which we can already distinguish with a 6 cm diameter telescope. The system lies at a distance of 54 light years. \ No newline at end of file diff --git a/en/star/hr5469.md b/en/star/hr5469.md deleted file mode 100644 index d1b73f1e5..000000000 --- a/en/star/hr5469.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Lup -constellation: Lup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:53:08.307344 ---- -the brightest star in the constellation. It varies in apparent brightness from 2.3mag to 2.8mag in a period of 0.260 days. It has a faint companion of 13.4mag. It is 460 light-years distant. \ No newline at end of file diff --git a/en/star/hr5497.md b/en/star/hr5497.md deleted file mode 100644 index ec8e82dd9..000000000 --- a/en/star/hr5497.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 54 Hya -constellation: Hya -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-06 11:43:44.158012 ---- -a binary star made up of 5.1mag and 7.1mag components that can be easily resolved by small telescopes at 8.6". Note the color of both stars, one is bright, the other is dark yellow. \ No newline at end of file diff --git a/en/star/hr5506.md b/en/star/hr5506.md deleted file mode 100644 index c95dd879c..000000000 --- a/en/star/hr5506.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Izar (ε Bootis) -constellation: Boo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 18:17:14.610098 ---- -Mirak or Pulcherrima - "beautiful". The second brightest star in the constellation is a beautiful double star in at least a 10cm telescope, consisting of an orange (2.7mag) and blue component (4.9mag) creating a colour contrast, at a distance of 2.9". But you'll need higher magnification and a quiet night. The distance of the system is 200 light years. \ No newline at end of file diff --git a/en/star/hr5523.md b/en/star/hr5523.md deleted file mode 100644 index a4ab57beb..000000000 --- a/en/star/hr5523.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: μ Lib -constellation: Lib -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:48:42.291162 ---- -double star, in a good 100 mm refractor we can see it as a close pair of white stars, like two disks in contact (1.8"). We can distinguish them completely during calm atmospheric conditions. The components have brightnesses of 5.8mag and 6.7mag. \ No newline at end of file diff --git a/en/star/hr5531.md b/en/star/hr5531.md deleted file mode 100644 index f65122fdb..000000000 --- a/en/star/hr5531.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Zubenelgenubi (α Lib) -constellation: Lib -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:46:41.081257 ---- -The name means "southern claw" and recalls the origin of the constellation. It is a very easily distinguishable double star, for which even a viewable telescope will suffice. At the main component of 2.75mag, there is a companion of 5.8mag at a distance of 231". In the binocular it is a bright wide pair consisting of a white and yellow component. Since both stars show the same proper motion, this is probably a true stellar pair. Its distance from Earth is 75 light years. \ No newline at end of file diff --git a/en/star/hr5544.md b/en/star/hr5544.md deleted file mode 100644 index 58f490e69..000000000 --- a/en/star/hr5544.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ξ Boo -constellation: Boo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 18:18:10.861770 ---- -a close binary star, with components of 4.8mag (yellow) with 6.9mag (red-orange), which have a mutual orbital period of 149 years. Since 1980, when they reached their greatest distance apart (7.2"), their separation has gradually decreased again, and is currently about 6". At their smallest separation of 1.8" (last seen in 1918), the guides are lost in small telescopes. The system is 22 light years away. Another star, HR 5553 (6mag), commonly appears in the field of view at a distance of 99" but is not related to this system. \ No newline at end of file diff --git a/en/star/hr5586.md b/en/star/hr5586.md deleted file mode 100644 index d85e6f098..000000000 --- a/en/star/hr5586.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Lib -constellation: Lib -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:48:19.247262 ---- -an occulting variable star similar to Algol, with a period of 2.32 days and a brightness range of 4.92-5.9mag. The entire cycle of brightness changes is therefore observable with the naked eye. The change from maximum to minimum takes place in about 6 hours, which can be noticed even on a spring night. There is one faint secondary minimum between the main minima, but it is only one tenth of the stellar size, so it is hardly noticeable. The system is nearly 300 light years from Earth. \ No newline at end of file diff --git a/en/star/hr5605.md b/en/star/hr5605.md deleted file mode 100644 index bb1123775..000000000 --- a/en/star/hr5605.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: π Lup -constellation: Lup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:54:40.826475 ---- -a nice system of almost equally bright pale blue stars, but one that requires quite a bit of magnification to distinguish. The stars lie only 1.4" apart. Their brightnesses are 4.6mag and 4.7mag. They lie at a distance of 440 light years. \ No newline at end of file diff --git a/en/star/hr5646.md b/en/star/hr5646.md deleted file mode 100644 index 48acde955..000000000 --- a/en/star/hr5646.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: κ Lup -constellation: Lup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:53:55.433114 ---- -a nice binary star whose white components with brightness 3.9mag and 5.8mag are 26.8" apart, so a telescope with a 5 cm objective is sufficient to resolve them. It is an optical binary only. \ No newline at end of file diff --git a/en/star/hr5652.md b/en/star/hr5652.md deleted file mode 100644 index 41ca9f277..000000000 --- a/en/star/hr5652.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ι Lib -constellation: Lib -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:47:49.569646 ---- -a complex multiple star that appears to be a single 4.2mag bright star when observed with the naked eye. Binocular will show its companion, referred to as 25 Librae. A telescope with a lens diameter over 80mm will reveal that the primary star has a faint 9mag guide at a distance of 58". A larger telescope and proper magnification should eventually prove it to be a tight binary as well. Its faint 11mag guide is at a distance of 1.9" from it. \ No newline at end of file diff --git a/en/star/hr5670.md b/en/star/hr5670.md deleted file mode 100644 index 60760ebc6..000000000 --- a/en/star/hr5670.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Cir -constellation: Cir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-24 19:47:40.393848 ---- -a main sequence star with a visual magnitude of 4.1mag that shines from a distance of 97 light years. \ No newline at end of file diff --git a/en/star/hr5683.md b/en/star/hr5683.md deleted file mode 100644 index 85c95d68a..000000000 --- a/en/star/hr5683.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: μ Lup -constellation: Lup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:54:20.419224 ---- -a triple star whose two main white components have magnitudes of 5.1mag and 5.2mag. They lie at a close distance of 1.2" and are a good test for a 100mm telescope. The brighter component has an additional yellow guide of 7.3mag, which is located at a distance of 23.7" from it and is visible even in a smaller telescope. \ No newline at end of file diff --git a/en/star/hr5685.md b/en/star/hr5685.md deleted file mode 100644 index c8f0f17b2..000000000 --- a/en/star/hr5685.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Zubenelschemali (β Lib) -constellation: Lib -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:46:14.804035 ---- -The "northern claw" is slightly brighter (2.61mag) and has a strange greenish tint, which is a bit unusual. The star is about 100 times brighter than the Sun. \ No newline at end of file diff --git a/en/star/hr569.md b/en/star/hr569.md deleted file mode 100644 index fe97e2128..000000000 --- a/en/star/hr569.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: λ Arietis -constellation: Ari -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:32:16.366362 ---- -a binary star very easily resolved in a 10 cm telescope. The yellow-white star (4.9mag) lies 37.4" from the pale blue component (7.7mag) \ No newline at end of file diff --git a/en/star/hr5694.md b/en/star/hr5694.md deleted file mode 100644 index 665730580..000000000 --- a/en/star/hr5694.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 5 Ser -constellation: Ser -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:27:13.253137 ---- -an unequally bright pair of yellow 5.1mag and reddish 10.1mag components 11.2" apart. A companion 9.1mag and the globular cluster M5 are in the field of view at a distance of 127". \ No newline at end of file diff --git a/en/star/hr5704.md b/en/star/hr5704.md deleted file mode 100644 index 4a52ff2ea..000000000 --- a/en/star/hr5704.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ Cir -constellation: Cir -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-24 19:48:07.625785 ---- -a binary star made up of magnitude 5.1 and 5.5 components only 0.6" apart. It is a good test for a 150 mm telescope. The components will orbit in 180 years. \ No newline at end of file diff --git a/en/star/hr5733.md b/en/star/hr5733.md deleted file mode 100644 index 3cd2830b8..000000000 --- a/en/star/hr5733.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alkalurops (μ Bootes) -constellation: Boo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 18:17:45.558821 ---- -easily distinguishable triple stars. Alongside the main yellow component (4.5mag), we see a 7.1mag companion at 108.3", which, when observed with at least an 8cm telescope, breaks into two stars about half a magnitude apart (7mag and 7.6mag) ( orange and yellow at 2.3" apart). \ No newline at end of file diff --git a/en/star/hr5735.md b/en/star/hr5735.md deleted file mode 100644 index 38582d1ff..000000000 --- a/en/star/hr5735.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Pherkad (γ UMi) -constellation: UMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:22:26.397611 ---- -The "blue and white" second wheel of the Little Chariot, near which is the orange star 11 Ursae minoris. The Arabs called them Pherkad - "two calves", later they began to distinguish Pherkad Maior (3.05 mag) and Pherkad Minor (5.02 mag). They form only an optical binary star, whose components are 480 and 390 light years apart, respectively. \ No newline at end of file diff --git a/en/star/hr5763.md b/en/star/hr5763.md deleted file mode 100644 index d69cc0762..000000000 --- a/en/star/hr5763.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ν Boo -constellation: Boo -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 18:18:36.004677 ---- -a double star distinguishable to the naked eye, consisting of an orange and a yellow-white component at a distance of 14'. Both stars are approximately 5mag. \ No newline at end of file diff --git a/en/star/hr5788.md b/en/star/hr5788.md deleted file mode 100644 index 247cbe11e..000000000 --- a/en/star/hr5788.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Ser -constellation: Ser -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:26:11.321523 ---- -the close pale yellow companions have a brightness of 4.2mag and 5.2mag. They orbit each other in a period of 3.170 years. We see them as a pair 4.4" apart in the sky. In a large telescope, we can see two more faint companions in close proximity with brightnesses of 14.7mag and 15mag. \ No newline at end of file diff --git a/en/star/hr5793.md b/en/star/hr5793.md deleted file mode 100644 index 2bdfffd59..000000000 --- a/en/star/hr5793.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Gemma (α CrB) -constellation: CrB -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:49:07.885144 ---- -Latin for "jewel". The Arabic name Alphecca (bowl) is more rarely used. The blue-white star, with a brightness of 2.3mag, is 75 ly away, and is 45 times brighter than the Sun. It's not visible to the naked eye, but it is an occulting variable star. It changes brightness by 0.1mag over 17.36 days. In space, it moves in the same direction as a group of stars mostly from the Big Dipper, known as the "Bear Stream". This group includes, for example, Sirius. \ No newline at end of file diff --git a/en/star/hr5812.md b/en/star/hr5812.md deleted file mode 100644 index 235e56d02..000000000 --- a/en/star/hr5812.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: τ Lib -constellation: Lib -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:47:02.445657 ---- -a pair of stars with brightnesses of 4.7mag and 9.7mag are separated by 8.5", so we can distinguish them with at least a 6 cm telescope. The system is 367 light years from Earth. \ No newline at end of file diff --git a/en/star/hr5834.md b/en/star/hr5834.md deleted file mode 100644 index a6d2e675c..000000000 --- a/en/star/hr5834.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ζ CrB -constellation: CrB -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:50:03.974676 ---- -nice double star even for a small telescope with a lens diameter of at least 6 cm. It consists of brightness components of 5.1mag and 6mag at a separation of 6.3 arcseconds. One component has a bluish tint, the other a greenish tint. It lies at a distance of 470 light years. \ No newline at end of file diff --git a/en/star/hr5854.md b/en/star/hr5854.md deleted file mode 100644 index 8c382a4aa..000000000 --- a/en/star/hr5854.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Unukalhai (α Ser) -constellation: Ser -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:25:15.613656 ---- -the brightest star in the constellation is 2.65mag. It is 74 light years from Earth and 35 times more luminous than the Sun. It belongs to the spectral class K2 and is an orange giant. \ No newline at end of file diff --git a/en/star/hr5867.md b/en/star/hr5867.md deleted file mode 100644 index 7d9d7cf0f..000000000 --- a/en/star/hr5867.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Ser -constellation: Ser -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:25:40.898336 ---- -a double star whose bright yellow and bluish yellow components have brightnesses of 3.7mag and 9.9mag, respectively, and lie 31" apart. We can therefore distinguish them with a small telescope. The system is 155ly from Earth. At a distance of 201" we can observe a component of 10.7mag. \ No newline at end of file diff --git a/en/star/hr5880.md b/en/star/hr5880.md deleted file mode 100644 index b93f7443b..000000000 --- a/en/star/hr5880.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R CrB -constellation: CrB -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:54:03.001927 ---- -the main representative of the working group of variable stars, in which a sudden drop in brightness of up to several stellar classes occurs at irregular intervals. The apparent brightness of this brilliant supergiant stays at 5.8mag most of the time, then drops to 13.8mag within a few weeks or sometimes to 15mag and stays that way for several months. This is because the supergiant ejects a huge cloud of carbon-rich gas by thermonuclear reaction into the surroundings, which obscures the star's light and causes the sharp drop in brightness we see. When the cloud dissipates, the star shines again with its light unabated. \ No newline at end of file diff --git a/en/star/hr5894.md b/en/star/hr5894.md deleted file mode 100644 index 8c84c032d..000000000 --- a/en/star/hr5894.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Ser -constellation: Ser -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:27:38.465566 ---- -a Mira-type variable star 10 degrees from Unukalhai between β and γ Ser, which reaches stellar magnitude 6 at its maximum, but is lost from the range of the binocular at its minimum as it drops to 13.4mag. The period of variation of its brightness is approximately 1 year - 357 days. \ No newline at end of file diff --git a/en/star/hr5897.md b/en/star/hr5897.md deleted file mode 100644 index bf2a0968e..000000000 --- a/en/star/hr5897.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β TrA -constellation: TrA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-03 08:07:00.475602 ---- -the main component of the 2.9mag luminosity has a faint 14mag guide at a distance of 155", but is not physically related to it. The brighter component has a white hue and is 40 light years away. \ No newline at end of file diff --git a/en/star/hr591.md b/en/star/hr591.md deleted file mode 100644 index fa227e40b..000000000 --- a/en/star/hr591.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: α Hyi -constellation: Hyi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.972802 ---- diff --git a/en/star/hr5925.md b/en/star/hr5925.md deleted file mode 100644 index 0eb556a5c..000000000 --- a/en/star/hr5925.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ξ Lup -constellation: Lup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:55:05.069650 ---- -bright, relatively wide pair (10.4"), easily distinguishable in small binoculars. The components have brightnesses of 5.3mag and 5.8mag, and observers perceive their colors differently: some see them as bright yellow, others say one is white and the other has a greenish tint. In general, stars with an AO spectrum appear white to pale blue. \ No newline at end of file diff --git a/en/star/hr5939.md b/en/star/hr5939.md deleted file mode 100644 index 3a6d08d40..000000000 --- a/en/star/hr5939.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: S TrA -constellation: TrA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-03 08:09:37.081529 ---- -another bright Cepheid. This time with a period of 6.323 days and a magnitude range of 6.1 to 6.7. \ No newline at end of file diff --git a/en/star/hr5948.md b/en/star/hr5948.md deleted file mode 100644 index 6d4178aef..000000000 --- a/en/star/hr5948.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: η Lup -constellation: Lup -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:53:34.755475 ---- -a triple star whose main component is blue-white and the guide is dark blue. The difference between their brightnesses is quite significant (3.6mag and 7.8mag), but with their 15" separation from each other, we should be able to distinguish them with a small telescope. The other companion 9.4mag lies 115" from the main component. Just to the northeast lie two 20" wide pairs of white stars. \ No newline at end of file diff --git a/en/star/hr5958.md b/en/star/hr5958.md deleted file mode 100644 index f24efb04f..000000000 --- a/en/star/hr5958.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: T CrB -constellation: CrB -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:48:34.002513 ---- -a variable star belonging to the recurrent novae, located southeast of η CRB. Two flares have been observed. In 1866, it increased its apparent brightness from 10.8mag to 2mag, and in the second outburst in 1946 it increased to only 3mag. At present, this star is only 10th magnitude. The star also occasionally explodes and ejects large amounts of gas. However, unlike the R CRB, it becomes very bright with each explosion. \ No newline at end of file diff --git a/en/star/hr596.md b/en/star/hr596.md deleted file mode 100644 index 0dfdfb2b1..000000000 --- a/en/star/hr596.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Al Rischa (α Psc) -constellation: Psc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.137365 ---- diff --git a/en/star/hr5961.md b/en/star/hr5961.md deleted file mode 100644 index 6f3ee3065..000000000 --- a/en/star/hr5961.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ι1 Nor -constellation: Nor -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.178864 ---- diff --git a/en/star/hr5978.md b/en/star/hr5978.md deleted file mode 100644 index e7ec2c121..000000000 --- a/en/star/hr5978.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ξ Sco -constellation: Sco -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:35:55.215248 ---- -a nice double star, with brightness components of 4.8mag and 7.3mag (bluish) at a distance of 7.6". The main star is also a binary, currently unobservable with a small telescope. The second component is almost as bright (5.1mag) and lies at a distance of only 0.5". It is yellow in colour. In the same field of view is Struve 1999, a dark yellow pair of 7.4mag and 8.1mag components, at a distance of 11.6". \ No newline at end of file diff --git a/en/star/hr5984.md b/en/star/hr5984.md deleted file mode 100644 index 97bb48e8a..000000000 --- a/en/star/hr5984.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Graffias (β Sco) -constellation: Sco -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:32:48.980000 ---- -it is a binary star with 2.6mag and 4.9mag components separated by 13.6". The main component is pale blue, the guide is dark blue, but there is no relationship between the two. The brighter component itself, however, is a close binary that is not easily distinguished even in a larger telescope. \ No newline at end of file diff --git a/en/star/hr599.md b/en/star/hr599.md deleted file mode 100644 index 62e6d7896..000000000 --- a/en/star/hr599.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Tri -constellation: Tri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 14:53:10.657090 ---- -an unequally bright binary with a brighter pale blue component (5.4mag) and a much fainter white companion (11.4mag). A (3.9") 200mm telescope can easily resolve them. \ No newline at end of file diff --git a/en/star/hr5993.md b/en/star/hr5993.md deleted file mode 100644 index bd274bdf5..000000000 --- a/en/star/hr5993.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ω Sco -constellation: Sco -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:34:50.746676 ---- -an optical binary visible to the naked eye, composed of stars of 3.9mag and 4.3mag. One is 470 and the other 290 light years away. \ No newline at end of file diff --git a/en/star/hr6008.md b/en/star/hr6008.md deleted file mode 100644 index e1818e6f7..000000000 --- a/en/star/hr6008.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Marfak (κ Her) -constellation: Her -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:22:58.732305 ---- -a physical binary whose yellow components of 5.3mag and 6.5mag are 28.4" apart and can therefore be distinguished even in small telescopes. \ No newline at end of file diff --git a/en/star/hr6020.md b/en/star/hr6020.md deleted file mode 100644 index 8a49bea9e..000000000 --- a/en/star/hr6020.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Aps -constellation: Aps -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:12:52.261278 ---- -a very wide binary star, easily distinguishable with a simple binocular. The magnitude 4.7 and 5.1 components are 103" apart, but are not physically related. They are red giants lying at distances of 660 and 760 light years. \ No newline at end of file diff --git a/en/star/hr6027.md b/en/star/hr6027.md deleted file mode 100644 index f5099ade6..000000000 --- a/en/star/hr6027.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ν Sco -constellation: Sco -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:35:26.680432 ---- - a four-pointed star, a small telescope can resolve two optical components at a distance of 44" with a brightness of 4.3mag and 6.4mag. The main star is already a true binary, the 6.8mag companion lies at a distance of only 0.9". The companion of the second star - a 7.8mag component - is located at a distance of 2.3" and is within the range of the 80 mm telescope. \ No newline at end of file diff --git a/en/star/hr603.md b/en/star/hr603.md deleted file mode 100644 index f502cebf1..000000000 --- a/en/star/hr603.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alamak (γ Adromedae) -constellation: And -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:07:40.431775 ---- -the star is 350 light years away. North of it lies the radiant of the Andromeda meteor shower. One of the most beautiful binary stars in the sky. The main component is orange and reaches a brightness of 2.3mag, the companion is green-blue and reaches 5.5mag and is also a close binary (0.5"), but imperceptible with smaller amateur instruments (in a larger telescope it appears as a fuzzy, somewhat elongated star). Its orbital period is 61 years. The angular distance between the main components of the alamak is 9.8 arc seconds, so a small telescope with a 5 cm diameter lens is sufficient to resolve them. \ No newline at end of file diff --git a/en/star/hr6063.md b/en/star/hr6063.md deleted file mode 100644 index e8ff0c3a9..000000000 --- a/en/star/hr6063.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: σ CrB -constellation: CrB -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:51:27.446305 ---- -The binary, a 5.6-mag main component, has a 6.6-mag companion at a distance of 7.1 arc seconds, which orbits it in 1,160 years. In a 100mm telescope we can easily distinguish the faint and inner dark components. \ No newline at end of file diff --git a/en/star/hr6072.md b/en/star/hr6072.md deleted file mode 100644 index 88700415d..000000000 --- a/en/star/hr6072.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: γ1 a γ2 Nor -constellation: Nor -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.889681 ---- diff --git a/en/star/hr6084.md b/en/star/hr6084.md deleted file mode 100644 index 23f61e08f..000000000 --- a/en/star/hr6084.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: σ Sco -constellation: Sco -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:33:24.703231 ---- -variable star, whose brightness varies between 3mag and 3.8mag over a period of 0.247 days, is also a binary star. The 9mag guide lies at a distance of 20" \ No newline at end of file diff --git a/en/star/hr6107.md b/en/star/hr6107.md deleted file mode 100644 index ffd56db7a..000000000 --- a/en/star/hr6107.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ν CrB -constellation: CrB -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:50:57.864773 ---- -a binary star whose red giant components of 5.2 and 5.4mag brightnesses are distinguishable by the binocular because they are spaced 370" apart. They are about 550 light years apart, but they do not orbit each other. \ No newline at end of file diff --git a/en/star/hr6112.md b/en/star/hr6112.md deleted file mode 100644 index 5e8feaae7..000000000 --- a/en/star/hr6112.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ρ Oph -constellation: Oph -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:55:34.377970 ---- -a binary star 3° northwest of Antares, consisting of blue components of 5.3mag and 6mag brightness at a distance of 3.1" (4.59mag). The area around them is of interest to photographers. To the west is the elongated dark Barnard 42 nebula, which appears silhouetted against the beautiful gas-dust complex IC 4604 , which is just irradiated by the star ρ Ophiuchi. However, the nebula has a very faint areal brightness. \ No newline at end of file diff --git a/en/star/hr6115.md b/en/star/hr6115.md deleted file mode 100644 index d6aa66ef8..000000000 --- a/en/star/hr6115.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ε Nor -constellation: Nor -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.979905 ---- diff --git a/en/star/hr6116.md b/en/star/hr6116.md deleted file mode 100644 index 1a2d78b02..000000000 --- a/en/star/hr6116.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: η UMi -constellation: UMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:22:58.202763 ---- -an optical binary whose main white component is 97 light-years away. When observed with the naked eye and a binocular, we can also see the other component, 19 Ursa minor, and its distant companion (5.5 mag), which is almost seven times farther away. \ No newline at end of file diff --git a/en/star/hr6134.md b/en/star/hr6134.md deleted file mode 100644 index e87be9aa9..000000000 --- a/en/star/hr6134.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Antares (α Sco) -constellation: Sco -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:32:19.885821 ---- -in antiquity, people saw this star as a competitor, the antipole of Mars (anti-Arés: against Mars), because the striking red star is very similar to the "Red Planet". The Old Arabic name Kal al Akrab is no longer used, but the Latin name Cor Scorpion - Heart of the Scorpion - is derived from it. It lies at the intersection of the elongated junctions of the sides of the Hercules quadrilateral. The physical guide, greenish in colour and 5.4mag in brightness, can be found at a distance of 2.9" preferably with 200mm and larger binoculars, as it is obstructed by the main star's glow. At least 250x magnification is recommended for visual resolution. It orbits the main component in approximately 555 years. \ No newline at end of file diff --git a/en/star/hr6149.md b/en/star/hr6149.md deleted file mode 100644 index b559826cc..000000000 --- a/en/star/hr6149.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: λ Oph -constellation: Oph -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:53:28.216905 ---- -a nice binary star with a period of 130 years. Its 4.2mag and 5.2mag components are located 1.5" apart. One of them is white, the other light yellow. At a greater distance, we can also observe two more, probably optical companions of 9.5mag and 11.1mag. \ No newline at end of file diff --git a/en/star/hr6163.md b/en/star/hr6163.md deleted file mode 100644 index 9c6f797ee..000000000 --- a/en/star/hr6163.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: β Aps -constellation: Aps -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:12:02.477429 ---- -a binary star consisting of a brighter 4.2mag component and a 12mag companion 51" away. It is probably an optical-only binary whose main component is of spectral class K0 and is 158 light years away. \ No newline at end of file diff --git a/en/star/hr617.md b/en/star/hr617.md deleted file mode 100644 index deee41802..000000000 --- a/en/star/hr617.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Hamal (α Aries) -constellation: Ari -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:30:58.320652 ---- -the brightest star in the constellation, otherwise unremarkable. This red giant of spectral class K2 reaches 2mag and shines at a distance of 66 light years. The star is sometimes referred to as El Nath. \ No newline at end of file diff --git a/en/star/hr6184.md b/en/star/hr6184.md deleted file mode 100644 index 6ac9071b1..000000000 --- a/en/star/hr6184.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 16/17 Dra -constellation: Dra -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:20:41.941797 ---- -a nice wide double star distinguishable in binoculars or small telescopes. The two components of nearly 5.5mag brightness are separated by 90.3". In fact, the 17 Dra component still has a close companion that lies 3.4" from it. All the stars are bright white. \ No newline at end of file diff --git a/en/star/hr6194.md b/en/star/hr6194.md deleted file mode 100644 index a2dba02ec..000000000 --- a/en/star/hr6194.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 36/37 Her -constellation: Her -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:23:27.678750 ---- -two ordinary nearby stars that we can distinguish with the binocular. They are located at the southwestern edge of the constellation at a mutual distance of 70" and their brightnesses are 5.7mag and 6.8mag, respectively. \ No newline at end of file diff --git a/en/star/hr6212.md b/en/star/hr6212.md deleted file mode 100644 index b91e6a73a..000000000 --- a/en/star/hr6212.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ζ Her -constellation: Her -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:18:27.799454 ---- -a nice potted double star. The components have magnitudes of 2.9mag and 5.5mag and are approximately 1.6" apart. Since their orbital period is only 34.5 years, the position angle and mutual distance change rapidly. \ No newline at end of file diff --git a/en/star/hr6217.md b/en/star/hr6217.md deleted file mode 100644 index 22c835e7d..000000000 --- a/en/star/hr6217.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Atria (α TrA) -constellation: TrA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-03 08:06:32.442806 ---- -the brightest star in the constellation has a brightness of 2 magnitude. The orange colour of this constellation is striking even when viewed with the naked eye. It lies 80 light years away. Its name, Atria, is an abbreviation of the words alpha Triangulo Australis, which was introduced by air navigators during World War II. \ No newline at end of file diff --git a/en/star/hr6247.md b/en/star/hr6247.md deleted file mode 100644 index d8a7e4d23..000000000 --- a/en/star/hr6247.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: μ Sco -constellation: Sco -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:34:00.595571 ---- -a binary star easily distinguishable to the naked eye. The brightness components 3.1mag and 3.6mag lie at a distance of 8'. The brighter of the two is an eclipsing binary whose brightness varies between 2.9 and 3.2mag over an interval of 34 hours. \ No newline at end of file diff --git a/en/star/hr6271.md b/en/star/hr6271.md deleted file mode 100644 index a0bf0e39c..000000000 --- a/en/star/hr6271.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ζ Sco -constellation: Sco -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:34:30.187630 ---- -a wide visual pair of unrelated stars distinguishable even with the naked eye. It consists of the blue-white giant ζ1, which is the brightest member (4.7mag) of the magnificent open cluster NGC 6231 . ζ2 is a red giant of 3.6mag, located at a much closer distance to us - 132ly. \ No newline at end of file diff --git a/en/star/hr6370.md b/en/star/hr6370.md deleted file mode 100644 index c71f982c6..000000000 --- a/en/star/hr6370.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alrakis (μ Dra) -constellation: Dra -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:21:54.386947 ---- -a well-known binary whose two white components have a brightness of about 5.65mag, but appear to the naked eye as a single 5th magnitude point. The mutual orbital period of the two partners is over 812 years. By the end of the 20th century, the two stars were about 1.9" apart and required higher magnification to separate them. This is therefore a good test for a good 100mm telescope. The system is 89 light years from Earth. \ No newline at end of file diff --git a/en/star/hr6402.md b/en/star/hr6402.md deleted file mode 100644 index 9afa45327..000000000 --- a/en/star/hr6402.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 36 Oph -constellation: Oph -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:55:58.780616 ---- -a beautiful double star of equally bright orange 5.1mag components, distinguishable at 4.9" in smaller telescopes. At a greater distance from it, an orange companion of 8.1mag brightness is still visible to the northwest. \ No newline at end of file diff --git a/en/star/hr6406.md b/en/star/hr6406.md deleted file mode 100644 index 79d168e78..000000000 --- a/en/star/hr6406.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Ras Algethi (α Her) -constellation: Her -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:21:30.994975 ---- -a bright red star almost on the border with Ophiuchus, a giant whose brightness varies irregularly between 3.1mag and 3.9mag, but often only between 3.3mag and 3.7mag. The period is 90 to 100 days. Suitable comparison stars are ι and κ Ophiuchi, which lie about 6.5 degrees to the southwest and have brightnesses of 4.3mag and 3.2mag, respectively. Alpha Herculis is also a binary whose second fifth-magnitude component, 4.7" away, is visible even in small telescopes with a 6 cm diameter objective. It has a greenish tint that contrasts nicely with the red giant. \ No newline at end of file diff --git a/en/star/hr6410.md b/en/star/hr6410.md deleted file mode 100644 index 6a096e0ae..000000000 --- a/en/star/hr6410.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Her -constellation: Her -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:18:48.335009 ---- -a well-known optical binary star whose faint blue components exhibit quite different proper motion, with the result that the relative positions of the two stars have changed quite significantly over time. In 1830 their mutual distance was 26", in 1960 they came as close as 9" and since then their distance has been gradually increasing again. The main star has a brightness of 3.1mag and the guide star 8.2mag. A telescope with a 6 cm diameter objective is sufficient to resolve this rare pair. \ No newline at end of file diff --git a/en/star/hr642.md b/en/star/hr642.md deleted file mode 100644 index 4d6a291f4..000000000 --- a/en/star/hr642.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 6 Tri -constellation: Tri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 14:52:27.067130 ---- -a physical binary whose seventh-magnitude companion can be distinguished from the fifth-magnitude primary using a small telescope. \ No newline at end of file diff --git a/en/star/hr6431.md b/en/star/hr6431.md deleted file mode 100644 index be50f00e0..000000000 --- a/en/star/hr6431.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 68 Her -constellation: Her -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:22:38.320163 ---- -an occulting variable star. It's actually two strongly flattened, nearly equal-sized stars that orbit each other in 2.051 days. As a result, we observe light changes in 68 Her from 4.7mag to 5.4mag. The luminosities of the two stars are quite different. The brighter is 260 times brighter than the Sun and the fainter is only 100 times brighter. Their masses are 7.5 and 2.9 times the mass of the Sun. In terms of size, the two stars are about 6 times the diameter of the Sun. \ No newline at end of file diff --git a/en/star/hr650.md b/en/star/hr650.md deleted file mode 100644 index d482d96a9..000000000 --- a/en/star/hr650.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 66 Cet -constellation: Cet -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 18:19:37.211853 ---- -the star is made up of two companions with a brightness of 5.7mag and 7.5mag. Their separation is 16.5 arc seconds. While in small telescopes it is a pair of yellow and blue components, in a 200 mm telescope the colour of the second component turns purple. \ No newline at end of file diff --git a/en/star/hr6536.md b/en/star/hr6536.md deleted file mode 100644 index 194c22444..000000000 --- a/en/star/hr6536.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Rastaban (β Dra) -constellation: Dra -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:17:53.741920 ---- -the star has a brightness of 2.8mag and is 380 light years away. Together with Etamine, they form the "dragon's eyes". Beta Draconis is a double star consisting of a main yellow component and a faint 14mag companion at an angular distance of 4.2", which is not easily seen. \ No newline at end of file diff --git a/en/star/hr6555.md b/en/star/hr6555.md deleted file mode 100644 index 70c162b6e..000000000 --- a/en/star/hr6555.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Kuma (ν Dra) -constellation: Dra -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:19:09.498753 ---- -a wide binary star composed of two nearly equally bright white stars (4.9mag) located 61.9" apart. Even observing this pair in trinary provides an exquisite view. The two components are 99 light years apart. \ No newline at end of file diff --git a/en/star/hr6556.md b/en/star/hr6556.md deleted file mode 100644 index 8e743b55b..000000000 --- a/en/star/hr6556.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Ras Alhague (α Oph) -constellation: Oph -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:53:05.674599 ---- -with its 2nd magnitude, it is the brightest star in the constellation. Ras Alhague lies at the northern edge of the constellation and is not very far from the star with a similar name, α Herculis, the main star of Hercules. It is a yellow-white giant 48 light years away. This distance is increasing due to its 8 km per second motion. \ No newline at end of file diff --git a/en/star/hr6623.md b/en/star/hr6623.md deleted file mode 100644 index 1d01faab7..000000000 --- a/en/star/hr6623.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: μ Her -constellation: Her -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-07 15:19:32.187322 ---- -the main and strikingly yellow 3.4mag component has a 10th magnitude companion at a distance of 33.8", which is actually made up of two red dwarfs. \ No newline at end of file diff --git a/en/star/hr6705.md b/en/star/hr6705.md deleted file mode 100644 index b1f0f81e2..000000000 --- a/en/star/hr6705.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Etamin (γ Dra) -constellation: Dra -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:17:35.298376 ---- -the brightest star in the constellation, reaching 2mag and apparently orange. It is 154 light years from Earth and 471 times brighter than the Sun. In the past, the English astronomer James Bradley also observed it and used it to discover the aberration of light. \ No newline at end of file diff --git a/en/star/hr6734.md b/en/star/hr6734.md deleted file mode 100644 index 7fe1474e2..000000000 --- a/en/star/hr6734.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: τ Oph -constellation: Oph -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:56:30.177615 ---- -a binary star that is made up of a nice but close pair of yellow stars of 5.2mag and 5.9mag brightness, with a period of 280 years. They are currently about 1.7" apart, but getting smaller. At a distance of 100" we can find a companion bright 9.3mag. \ No newline at end of file diff --git a/en/star/hr6752.md b/en/star/hr6752.md deleted file mode 100644 index d72a67ac2..000000000 --- a/en/star/hr6752.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 70 Oph -constellation: Oph -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:54:01.341332 ---- -a binary star consisting of two stars of brightness 4.2mag and 6mag with a mutual orbital period of 87 years. The orbit has such a spatial position that the apparent angular separation of the two stars changes significantly during the orbital period. The smallest separation (1.5") was reached by the two stars in 1989 and 1990. By the turn of the millennium, their separation had increased to 3.9", which was enough for a telescope with a 5 cm diameter lens. In 2005, the distance was increased to 5". The two stars will reach their greatest ever separation of 6.8" in 2024. \ No newline at end of file diff --git a/en/star/hr6783.md b/en/star/hr6783.md deleted file mode 100644 index 557fb1f93..000000000 --- a/en/star/hr6783.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Tel -constellation: Tel -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 10:51:00.055403 ---- -A binary star consisting of a 4.5mag main component and a faint 13mag companion located 21" away. The components are 410 light years apart. \ No newline at end of file diff --git a/en/star/hr681.md b/en/star/hr681.md deleted file mode 100644 index 9e1930ece..000000000 --- a/en/star/hr681.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Mira Ceti (ο Cet) -constellation: Cet -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 18:17:12.478262 ---- -the best-known long-period variable star, which on 13 August 1596 was thought by the Dutch amateur observer David Fabricius in Germany to be a new star, similar to the recent Tycho's Star of 1572. In fact, no star of magnitude 3 was plotted in the neck of the Whale in any atlas of that time or earlier. It was not until observing it during the following year that he discovered that it was changing its brightness. He was thus the first to discover the first variable star in the history of astronomy, in the days of Galileo before the invention of the telescope! The star gradually disappeared and reappeared until in 1603 the German astrocartographer Johann Bayer plotted it in his atlas as a 4th magnitude object. Later, in 1662, Jan Hevelius named it "Mira stella" - the wondrous star. It is pointed at by the tip of the letter "V", which is formed by the stars of the constellation Pisces. Mira is 300 light years away. \ No newline at end of file diff --git a/en/star/hr6832.md b/en/star/hr6832.md deleted file mode 100644 index d3f56a8de..000000000 --- a/en/star/hr6832.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: η Sgr -constellation: Sgr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:37:01.486258 ---- -an easy-to-observe binary: the magnitudes of the components are 3.2 and 7.8 and lie at distances of 3.6". The brighter component is red-orange, the fainter one is white. At a distance of 93" lies a 10mag star, and at a distance of 33" a 13mag star. \ No newline at end of file diff --git a/en/star/hr6855.md b/en/star/hr6855.md deleted file mode 100644 index 3ab0a80ce..000000000 --- a/en/star/hr6855.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ξ Pav -constellation: Pav -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.604252 ---- diff --git a/en/star/hr6879.md b/en/star/hr6879.md deleted file mode 100644 index 2d84daeb6..000000000 --- a/en/star/hr6879.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Kaus Australis (ε Sgr) -constellation: Sgr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:36:36.184446 ---- -the brightest star in the constellation (1.85mag). It is located in the southern part of the bow and reaches a maximum height of 7 degrees above the southern horizon at the time of culmination. It is white in colour. At a distance of 125 light years it shines like 250 suns. It is also an optical double star, and to the northwest about 3.3 arc minutes is a seventh magnitude guide star, which we can discover by binocular. \ No newline at end of file diff --git a/en/star/hr6896.md b/en/star/hr6896.md deleted file mode 100644 index 078335bf6..000000000 --- a/en/star/hr6896.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 21 Sgr -constellation: Sgr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:38:14.269343 ---- -An unequally bright and contrasting double star of orange (4.9mag) and bluish component (7.4mag), which lie only 1.8" apart, so they are not easily distinguishable with a small telescope. \ No newline at end of file diff --git a/en/star/hr6897.md b/en/star/hr6897.md deleted file mode 100644 index 5ffbdc884..000000000 --- a/en/star/hr6897.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Tel -constellation: Tel -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 10:50:29.797662 ---- -the brightest star in the constellation reaches a brightness of 3.76mag. It is a blue-white star of spectral class B3, 249 light-years away. \ No newline at end of file diff --git a/en/star/hr6918.md b/en/star/hr6918.md deleted file mode 100644 index f036d9ea8..000000000 --- a/en/star/hr6918.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 59 Ser -constellation: Ser -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:28:06.642624 ---- -an unequally bright but attractive double star with a yellow 5.3mag and white 7.6mag component located in a particularly dark region of the Great Rift. The mutual separation of this pair is 3.8". \ No newline at end of file diff --git a/en/star/hr6923.md b/en/star/hr6923.md deleted file mode 100644 index 7c339e264..000000000 --- a/en/star/hr6923.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 39 Dra -constellation: Dra -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:20:13.336570 ---- -a multiple star, which a small telescope and even a binocular show as a wide pair of stars with 5mag and 8mag brightness. Inspection of the brighter star at high magnification reveals yet another (and much closer) component that also reaches 8mag. \ No newline at end of file diff --git a/en/star/hr6934.md b/en/star/hr6934.md deleted file mode 100644 index c4e5ff79b..000000000 --- a/en/star/hr6934.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Tel -constellation: Tel -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 10:52:33.868182 ---- -an optical binary easily distinguishable to the naked eye. It is made up of 4.9mag and 5.1mag brightness components 800 and 1 100 light years away. \ No newline at end of file diff --git a/en/star/hr6953.md b/en/star/hr6953.md deleted file mode 100644 index 7693b6b4a..000000000 --- a/en/star/hr6953.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: κ CrA -constellation: CrA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:45:09.341279 ---- -a remarkable binary star in the rich Milky Way, whose two blue-white companions, 5.9mag and 6.6mag, are 21.4 arc seconds apart. They are therefore easy to distinguish even in a small telescope. \ No newline at end of file diff --git a/en/star/hr7001.md b/en/star/hr7001.md deleted file mode 100644 index b24c43c5c..000000000 --- a/en/star/hr7001.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Vega (α Lyr) -constellation: Lyr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:44:01.932942 ---- -This star makes the constellation unmissable, as bluish Vega is the fifth brightest star in the sky (0.04mag). Together with the stars Deneb in Cygnus and Altair in Aquila, Vega forms the Summer Orientation Triangle. Its distance from Earth is determined to be 25ly and its luminosity is 40 times that of our Sun, absolute magnitude = +0.5. The two faint companions do not form part of a physical system. \ No newline at end of file diff --git a/en/star/hr7020.md b/en/star/hr7020.md deleted file mode 100644 index 647110e7e..000000000 --- a/en/star/hr7020.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Sct -constellation: Sct -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:44:32.267776 ---- -this star is the prototype of a class of variable stars whose brightness changes little due to repeated decreasing and increasing diameter with a period of a few hours. Over a period of 4.65 hours, its brightness fluctuates between 4.9mag and 5.2mag. δ Scuti also has a 52.6" blue guide star at 52.6" distance that contrasts nicely with the main, bright yellow star. \ No newline at end of file diff --git a/en/star/hr7051.md b/en/star/hr7051.md deleted file mode 100644 index 5429a0585..000000000 --- a/en/star/hr7051.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Lyrae -constellation: Lyr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:50:26.574802 ---- -A "double binary", a multiple system near Vega in which we can already distinguish two components with our sharp eyes. In the binocular, these components are clearly distinguishable, brightnesses of 5.1mag and 5.4mag at a distance of 208", which, when observed with at least a 60 mm telescope and higher magnification, disintegrate into double stars (guides ε1 6.5mag and ε2 5.3mag). The mutual distance of one pair is 2.6", the other 2.3", and their orbital periods are determined to be 1 166 and 585 years, respectively. The distances are 162ly and 156ly. \ No newline at end of file diff --git a/en/star/hr7066.md b/en/star/hr7066.md deleted file mode 100644 index 6879fd941..000000000 --- a/en/star/hr7066.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Scuti -constellation: Sct -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:45:13.352809 ---- -Dark yellow giant, semi-regular variable star of the RV Tauri type, one degree south of β Scuti (4.2 mm). Its brightness varies from 4.9mag to 8.2mag over a period of five months - a main period of 140 days. The cause of the deep minimum may be carbon particles formed in the star's atmosphere. It is within range of the binocular, being the brightest variable star of the RV Tauri type: it appears to oscillate in at least two overlapping periods, and at its maximum it is at least 8,000 times more luminous than the Sun. It often changes brightness between 5-6mag, but after four or five such cycles it drops to 8th magnitude. It is about 2,500 light years away. Similar stars have been found not only in parts of the Milky Way, but also in globular clusters, whether in the very centre of the Galaxy. \ No newline at end of file diff --git a/en/star/hr707.md b/en/star/hr707.md deleted file mode 100644 index 910bbae72..000000000 --- a/en/star/hr707.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ι Cas -constellation: Cas -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:12:46.778944 ---- - one of the most beautiful triple stars in the sky. The main, white star of 4.7mag is accompanied by a yellow and blue component. At a distance of 2.3" is the first 7mag guide. At a distance of 7.2" is the second component associated with this system, with a brightness of 8.4mag. The components of the main AB pair orbit each other in 840 years. \ No newline at end of file diff --git a/en/star/hr7106.md b/en/star/hr7106.md deleted file mode 100644 index fb75ccaa2..000000000 --- a/en/star/hr7106.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Sheliak (β Lyr) -constellation: Lyr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:44:31.113620 ---- -is a representative of the occultation variable beta Lyra type stars. The two stars orbiting each other have the shape of a rotating ellipsoid. The star changes brightness from 3.4mag to 4.4mag over a period of 12.908 days. Within the period, there is also a secondary minimum at which the brightness drops by 0.4mag. Suitable comparison stars are γ (3.25mag) and κ LYR (4.33mag). \ No newline at end of file diff --git a/en/star/hr7107.md b/en/star/hr7107.md deleted file mode 100644 index 6a4b7a8b2..000000000 --- a/en/star/hr7107.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: κ Pav -constellation: Pav -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.747606 ---- diff --git a/en/star/hr7139.md b/en/star/hr7139.md deleted file mode 100644 index 32f43c4f2..000000000 --- a/en/star/hr7139.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Lyr -constellation: Lyr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:46:33.846352 ---- -an easily observable optical binary at a distance of 620", one component of which is colored strongly red (with slightly variable brightness ranging from 4.3 to 4.4mag) and the other pale blue (5.5mag). They can be distinguished by a binocular. \ No newline at end of file diff --git a/en/star/hr7141.md b/en/star/hr7141.md deleted file mode 100644 index 927094038..000000000 --- a/en/star/hr7141.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alya (θ Ser) -constellation: Ser -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:26:35.104696 ---- -a double star at the eastern edge of the constellation. The pair of blue-white stars, 4.6mag and 5.1mag, are 22.3" apart, so a conventional binocular will be sufficient to distinguish them. Both belong to spectral class A5 and are physically related. They lie at a distance of 86ly. \ No newline at end of file diff --git a/en/star/hr7152.md b/en/star/hr7152.md deleted file mode 100644 index b65a50c20..000000000 --- a/en/star/hr7152.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε CrA -constellation: CrA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:43:16.722060 ---- -an occulting variable star with a period of 14 hours. Since it lies on the northern edge of the constellation, it can be seen here, at least from areas at higher altitudes and without light pollution. \ No newline at end of file diff --git a/en/star/hr7157.md b/en/star/hr7157.md deleted file mode 100644 index 2e89b1c3f..000000000 --- a/en/star/hr7157.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Lyrae -constellation: Lyr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:44:55.475423 ---- -the striking red-orange star visible to the naked eye is a semi-regular variable star whose brightness varies from 3.8mag to 5mag over approximately 46 days. \ No newline at end of file diff --git a/en/star/hr7226.md b/en/star/hr7226.md deleted file mode 100644 index d384d6c04..000000000 --- a/en/star/hr7226.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ CrA -constellation: CrA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-25 15:44:39.741765 ---- -a close binary whose equally bright 5-mag components orbit each other in 120 years. We can only make them out with a larger telescope. It lies 58 light years away. \ No newline at end of file diff --git a/en/star/hr7228.md b/en/star/hr7228.md deleted file mode 100644 index 504bfa9ad..000000000 --- a/en/star/hr7228.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: σ Octantis -constellation: Oct -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.325322 ---- diff --git a/en/star/hr7243.md b/en/star/hr7243.md deleted file mode 100644 index b21100bac..000000000 --- a/en/star/hr7243.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Aquilae -constellation: Aql -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:25:36.936050 ---- -a Mira-type variable star located in the Milky Way 5.5 degrees south of ζ Aquilae. Since the beginning of the 20th century, the period of brightness variation of this red supergiant has shortened by about 66 days. At the beginning of the 20th century, the period lasted about 350 days. Currently, the brightness changes from 5.5mag to 11.5mag in 284 days. \ No newline at end of file diff --git a/en/star/hr7296.md b/en/star/hr7296.md deleted file mode 100644 index 2229e47fa..000000000 --- a/en/star/hr7296.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: RY Sgr -constellation: Sgr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:39:18.136923 ---- -similar to R Coronae Borealis, because it suddenly and unexpectedly changes its brightness from eighth to fourteenth magnitude. It has no precise period and is the brightest star of this type after R Coronae Borealis itself. Its brightness drops unexpectedly when carbon soot builds up in the atmosphere. \ No newline at end of file diff --git a/en/star/hr7326.md b/en/star/hr7326.md deleted file mode 100644 index cfd5ade86..000000000 --- a/en/star/hr7326.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: U Sge -constellation: Sge -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:31:33.817351 ---- -over a period of 3.38 days, the brightness of this occultation variable star of the Algol type varies from 6.6mag to 9.2mag. It is a suitable object for small telescopes because the changes near the beginning and end of the minimum can be seen within a few minutes. The eclipse, which occurs once every three and a half days or so, lasts about an hour and forty minutes. The main component is the blue star of the main sequence, while the larger but fainter guide is the yellow giant. \ No newline at end of file diff --git a/en/star/hr7337.md b/en/star/hr7337.md deleted file mode 100644 index a8327d9fa..000000000 --- a/en/star/hr7337.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Arkab (β Sgr) -constellation: Sgr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:37:34.043226 ---- -a wide optical binary suitable for binocular observations. The 3.9mag main component also has an 8th magnitude companion at 28.4". \ No newline at end of file diff --git a/en/star/hr7417.md b/en/star/hr7417.md deleted file mode 100644 index 70d4b809d..000000000 --- a/en/star/hr7417.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Albireo (β Cygni) -constellation: Cyg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:51:44.054210 ---- -forms the head of the Swan or the lower end of the cross and is one of the most beautiful contrasting double stars. Since the orbit of the fainter star around the brighter one cannot be directly observed, it cannot be said with certainty that it is a physical binary. The system is approximately 400ly away. The main component is 950 times and the secondary 230 times brighter than the Sun. \ No newline at end of file diff --git a/en/star/hr7476.md b/en/star/hr7476.md deleted file mode 100644 index 7816d01fe..000000000 --- a/en/star/hr7476.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 54 Sgr -constellation: Sgr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:38:36.505178 ---- -nice triple stars easily distinguishable in small telescopes. The brightest component is dark yellow (5.4mag), the next is pale blue (11.9mag) and the third is yellowish (8.9mag). Pair spacing AB is 38", component spacing AC = 45.6". \ No newline at end of file diff --git a/en/star/hr7479.md b/en/star/hr7479.md deleted file mode 100644 index 63e0ae6c1..000000000 --- a/en/star/hr7479.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Sham (α Sge) -constellation: Sge -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:29:58.467834 ---- -The name, introduced about 200 years ago by Giuseppe Piazza, the Italian astronomer who, among other things, discovered the first planet Ceres, is based on the Old Arabic name Sahm - arrow. This yellow giant of spectral class G0 has a brightness of 4.4mag and is 382ly distant. It has four faint guides. \ No newline at end of file diff --git a/en/star/hr749.md b/en/star/hr749.md deleted file mode 100644 index b4989bfdc..000000000 --- a/en/star/hr749.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ω For -constellation: For -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.680841 ---- diff --git a/en/star/hr7528.md b/en/star/hr7528.md deleted file mode 100644 index 899e45b64..000000000 --- a/en/star/hr7528.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Cygni -constellation: Cyg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:51:06.031621 ---- -a binary star, the magnitudes of the components are 2.9 and 6.3, their separation is 2.4" and their distance from Earth is 124ly. It is a good test for a 10-15 cm telescope. The main component is reported by observers as white, pale blue or even blue-green, the minor component appears pale blue to blue. \ No newline at end of file diff --git a/en/star/hr7544.md b/en/star/hr7544.md deleted file mode 100644 index 507fd79db..000000000 --- a/en/star/hr7544.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: π Aquilae -constellation: Aql -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:27:04.123398 ---- -a couple of nice yellow stars (6.1mag and 6.9mag) at a distance of 1.4" can be seen with a 10 cm telescope, but at 150x magnification they are still in contact with each other. \ No newline at end of file diff --git a/en/star/hr7546.md b/en/star/hr7546.md deleted file mode 100644 index 3586ddfad..000000000 --- a/en/star/hr7546.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ζ Sge -constellation: Sge -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:30:26.859369 ---- -the 5.5mag main star has a guide star of 8.7mag at 8.6". In smaller telescopes this unequally bright pair is closely separated. The main star is a physical binary, indistinguishable by amateur telescopes - it appears as a bright yellow, the guide is blue. The system is 260ly distant. At a distance of 76" there is a fourth star in the sky, 11mag. \ No newline at end of file diff --git a/en/star/hr7557.md b/en/star/hr7557.md deleted file mode 100644 index dbf350af4..000000000 --- a/en/star/hr7557.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Altair (α Aquilae) -constellation: Aql -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:24:04.046238 ---- - one of the closest bright stars visible to the naked eye. It has a brightness of 0.77mag, and is approximately 16.5 light years away. It's only 11 times brighter and one and a half times larger in diameter than our sun. Altair is also an optical binary star, at a distance of 165 arc seconds there is a 10mag companion, still visible with an 8cm telescope. \ No newline at end of file diff --git a/en/star/hr7564.md b/en/star/hr7564.md deleted file mode 100644 index 5867edac9..000000000 --- a/en/star/hr7564.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: χ Cygni -constellation: Cyg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:52:37.099667 ---- -at its maximum of 3mag to 5mag, this long-period variable star located in the southwestern part of the constellation is visible to the naked eye, while in 6 to 7 months or up to 406 days it reaches its minimum around 13th to 14th mag. It is the brightest star of this type after Mira Ceti itself. A suitable comparison star is η Cygni (3.89mag). \ No newline at end of file diff --git a/en/star/hr7570.md b/en/star/hr7570.md deleted file mode 100644 index ad92cf20f..000000000 --- a/en/star/hr7570.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: η Aquilae -constellation: Aql -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:24:34.785146 ---- -The brightest Cepheid in the sky, 1,000 light years away, lies 8 degrees south of Altair. Changes in the brightness of this supergiant are easily perceived with the naked eye. In 7 days and 4 hours, its brightness fluctuates regularly between 3.7mag and 4.4mag. It is useful to compare its brightness variations with θ, δ (3mag) and λ (4mag) stars. \ No newline at end of file diff --git a/en/star/hr758.md b/en/star/hr758.md deleted file mode 100644 index 030e06796..000000000 --- a/en/star/hr758.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Trianguli -constellation: Tri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 14:52:47.948206 ---- -a variable star of the type Mira Ceti with magnitude variations from 5.7 to 12.6 and a period of 267 days. \ No newline at end of file diff --git a/en/star/hr7635.md b/en/star/hr7635.md deleted file mode 100644 index f1dfb922e..000000000 --- a/en/star/hr7635.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ Sge -constellation: Sge -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:29:37.588717 ---- -the brightest star in the constellation with an apparent brightness of 3.71mag. An orange giant of spectral class K5, shining from a distance of about 258ly. \ No newline at end of file diff --git a/en/star/hr7705.md b/en/star/hr7705.md deleted file mode 100644 index cb5cbd7d4..000000000 --- a/en/star/hr7705.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: θ Sge -constellation: Sge -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:31:00.895822 ---- -a triple star, observed along the southwestern boundary of the inconspicuous open cluster NGC 6873, which is in the same field of view in a larger telescope. In the 100mm telescope, the AB components appear pale yellow (6.5mag), and a third, orange star of 9mag brightness is located at 84". \ No newline at end of file diff --git a/en/star/hr7754.md b/en/star/hr7754.md deleted file mode 100644 index 40a37ac9b..000000000 --- a/en/star/hr7754.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Prima Giedy (α1 Cap) -constellation: Cap -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 22:07:48.826160 ---- -with a brightness of 4.2mag, it is, together with α2 (Secunda Giedo - 3.6mag), an optical binary, in favourable conditions distinguishable with the naked eye, at the northwest corner of the "triangular" constellation. In fact, the components lie 378 arc seconds apart, which is about 1/5 the diameter of the full Moon. Prima Giedo is the giant 117 light years away, while the giant Secunda Giedo lies closer, at a distance of about 102 light years. However, they are a pretty pair of two orange-yellow stars in the sky. \ No newline at end of file diff --git a/en/star/hr7776.md b/en/star/hr7776.md deleted file mode 100644 index a4210758a..000000000 --- a/en/star/hr7776.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Dabih Major (β Cap) -constellation: Cap -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 22:07:18.128340 ---- -It's a yellow spectral binary of 3.3mag brightness with an invisible companion that orbits it in 1374 days, 650ly away. At a distance of 205" is the bluish companion Dabih Minor - β1, of 6mag brightness. It lies at a distance of 328 light years. The whole system is illustrated by a third, yellow 9mag star and, in larger telescopes, a faint pair of 13mag stars. \ No newline at end of file diff --git a/en/star/hr7790.md b/en/star/hr7790.md deleted file mode 100644 index a8597b7e1..000000000 --- a/en/star/hr7790.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Peacock (α Pavi) -constellation: Pav -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.237744 ---- diff --git a/en/star/hr7796.md b/en/star/hr7796.md deleted file mode 100644 index 59b55fe80..000000000 --- a/en/star/hr7796.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Sadr (γ Cygni) -constellation: Cyg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:50:36.521693 ---- -the star has a guide star, which, with a magnitude of 9.9 at a distance of 142", can be seen with a telescope with a 6 cm diameter lens. He himself is still a close binary. The distance from the Earth is estimated to be 1800ly, so its luminosity is 33,000 times that of the Sun. \ No newline at end of file diff --git a/en/star/hr7814.md b/en/star/hr7814.md deleted file mode 100644 index 96c52ea66..000000000 --- a/en/star/hr7814.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: π Cap -constellation: Cap -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 22:08:53.181778 ---- -a binary star consisting of two components of 5.3mag and 8.9mag brightness at a distance of 3.2". To resolve them, we will need a telescope with an objective lens diameter of at least 10 cm and an eyepiece with a shorter focal length. After all, even at 200mm and 200x magnification, there is only a tight pair of pale and blue components. \ No newline at end of file diff --git a/en/star/hr7822.md b/en/star/hr7822.md deleted file mode 100644 index 927d315fa..000000000 --- a/en/star/hr7822.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ρ Cap -constellation: Cap -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 22:08:27.453589 ---- -quite a nice double star even in binoculars and small telescopes. The stars (5mag, 6.7mag) lie 247.6" apart, and therefore become a wide colored pair of yellow and magenta stars in a 15 cm telescope. \ No newline at end of file diff --git a/en/star/hr7869.md b/en/star/hr7869.md deleted file mode 100644 index 5abe5cb6c..000000000 --- a/en/star/hr7869.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: α Ind -constellation: Ind -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.399805 ---- diff --git a/en/star/hr7924.md b/en/star/hr7924.md deleted file mode 100644 index 2f6d12ad6..000000000 --- a/en/star/hr7924.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Deneb (α Cygni) -constellation: Cyg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:49:42.592073 ---- -the brightest star in the constellation, which, along with Vega in Lyra to the west and Altair in Orleus to the south, forms the Summer Triangle of Orientation. This bright blue-white supergiant (1.2mag) is much further away than other bright stars in our sky - it lies at a distance of 2600ly. To be this bright from this distance, Deneb must have an energy output greater than 60,000 Suns, making it one of the brightest stars visible to the naked eye (e.g. Vega is 25 and Altair only 11 light years away). Its mass is 19 times and its diameter 203 times that of the Sun. The surface temperature reaches 8500K. \ No newline at end of file diff --git a/en/star/hr7948.md b/en/star/hr7948.md deleted file mode 100644 index f89d01f65..000000000 --- a/en/star/hr7948.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ1,2 Del -constellation: Del -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:56:20.149146 ---- -a physical binary star whose apparent brightness components of 4.3mag (yellow) and 5.1mag (greenish) are 10" apart in the sky, so we can distinguish them in a 5 cm telescope. The guide might also appear bluish in some eyepieces, due to the contrast with the yellow main component. \ No newline at end of file diff --git a/en/star/hr7965.md b/en/star/hr7965.md deleted file mode 100644 index 2ccf91f88..000000000 --- a/en/star/hr7965.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: α Mic -constellation: Mic -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.030675 ---- diff --git a/en/star/hr8034.md b/en/star/hr8034.md deleted file mode 100644 index 55899ff15..000000000 --- a/en/star/hr8034.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Equ -constellation: Equ -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:41:55.342997 ---- -a binary star with a component magnitude of 6mag at a separation of 0.8" and a true orbit of approximately 101.4 years. At low magnification they merge into a single bright yellow star that contrasts nicely with a single 7mag blue star in the same field of view (10.7"). Still at 200x in a 200mm scope, the two main components show up as an extended line. Moreover, the brighter of the two components is actually a physical binary star with an orbital period of 100 years, but the components are too close together to separate with a small telescope. \ No newline at end of file diff --git a/en/star/hr8039.md b/en/star/hr8039.md deleted file mode 100644 index 9133b9fef..000000000 --- a/en/star/hr8039.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: γ Mic -constellation: Mic -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.000880 ---- diff --git a/en/star/hr804.md b/en/star/hr804.md deleted file mode 100644 index 055fbd106..000000000 --- a/en/star/hr804.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Kaffaljidhma (γ Cet) -constellation: Cet -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 18:17:59.670995 ---- -a beautiful close physical binary star resolved in a 100 mm telescope, with a yellow 3.5mag and white 7.3mag component. It lies at a distance of 2.8". The mutual orbital period of this pair is expected to be about several millennia. A 10th-magnitude red dwarf, also part of the system, is added in the 200 mm telescope. It lies at a distance of 14'. The entire system is about 80 light years away. \ No newline at end of file diff --git a/en/star/hr8085.md b/en/star/hr8085.md deleted file mode 100644 index 452f29c9f..000000000 --- a/en/star/hr8085.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 61 Cygni -constellation: Cyg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-27 17:53:41.993397 ---- -this inconspicuous binary star, recognizable even with a smaller telescope, is famous for being the first to have its trigonometric parallax measured in 1838 - the distance of this constellation was determined by the German astronomer Friedrich Wilhelm Bessel (he worked mainly in astrometry - he measured precisely the positions of over 50,000 stars and predicted the presence of their long-invisible guides in 1844 on the basis of an analysis of the irregular proper motion of the magnitude and Procyon). \ No newline at end of file diff --git a/en/star/hr8097.md b/en/star/hr8097.md deleted file mode 100644 index 1dd28937d..000000000 --- a/en/star/hr8097.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ/6 Equ -constellation: Equ -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:41:13.022865 ---- -only an optical binary star, on a good night distinguishable to the naked eye. The stars (4.6mag, 6mag) lie almost 6 arc minutes apart. However, Gamma EQU also has an 11th mag physical companion that lies 2" apart. At least a 150mm telescope is needed to see it. They are 118 light years away. \ No newline at end of file diff --git a/en/star/hr8131.md b/en/star/hr8131.md deleted file mode 100644 index a7e39f03f..000000000 --- a/en/star/hr8131.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Kitalpha (α Equ) -constellation: Equ -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-10 16:40:48.313240 ---- - is the brightest star in the constellation, although it only reaches 3.92mag. The other stars in the constellation are already below 4th magnitude. Kitalpha is a yellow giant of spectral class G0, from which light has been traveling to us for 186 years. \ No newline at end of file diff --git a/en/star/hr8140.md b/en/star/hr8140.md deleted file mode 100644 index 4fc7f0947..000000000 --- a/en/star/hr8140.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: θ Ind -constellation: Ind -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.571050 ---- diff --git a/en/star/hr815.md b/en/star/hr815.md deleted file mode 100644 index 4d30fc39f..000000000 --- a/en/star/hr815.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: RZ Cassiopeiae -constellation: Cas -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:14:04.469176 ---- -an interesting occulting variable star. The period of brightness changes is 1.19 days, but the drop in brightness from 6.18mag to 7.72mag lasts only two hours, while brightening then occurs immediately and the star returns to its original magnitude in another two hours. \ No newline at end of file diff --git a/en/star/hr8151.md b/en/star/hr8151.md deleted file mode 100644 index 6af4d4574..000000000 --- a/en/star/hr8151.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: θ Mic -constellation: Mic -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.296259 ---- diff --git a/en/star/hr8162.md b/en/star/hr8162.md deleted file mode 100644 index c4ef1414b..000000000 --- a/en/star/hr8162.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alderamin (α Cep) -constellation: Cep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 13:37:13.967876 ---- -the brightest star in the constellation at 2.44mag. It is a yellow-white star of spectral class A7, 49 light-years away, forming the constellation's rhombus along with β (3.21mag), ζ (3.35mag) and ι (3.52mag). At its centre lies the star ξ Cep. Alderamin becomes the closest star to the north celestial pole around 7500 AD due to precession of the Earth's axis. It has 17 times the luminosity of the Sun. \ No newline at end of file diff --git a/en/star/hr8238.md b/en/star/hr8238.md deleted file mode 100644 index f2a5d1731..000000000 --- a/en/star/hr8238.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Alfirk (β Cep) -constellation: Cep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 13:37:51.531863 ---- -a binary star resolvable in a small telescope with a 6 cm diameter objective lens, consisting of two components of 3.2mag (bright white) and 7.9mag (blue - emerald green in a large telescope) at a mutual distance of 13.3". The main star is also a spectroscopic binary, with an orbital period of only 4 and 3/4 hours. At the same period it shows a slight change in brightness between 3.3mag and 3.4mag. It is even the prototype of a group of variable stars called beta Cepheids, whose brightness variations are so small that they are barely perceptible to the eye. It lies at a distance of 690 light years. \ No newline at end of file diff --git a/en/star/hr8254.md b/en/star/hr8254.md deleted file mode 100644 index c9cc41c0f..000000000 --- a/en/star/hr8254.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ν Oct -constellation: Oct -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.051386 ---- diff --git a/en/star/hr8280.md b/en/star/hr8280.md deleted file mode 100644 index 47a880729..000000000 --- a/en/star/hr8280.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: λ Oct -constellation: Oct -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.493530 ---- diff --git a/en/star/hr8308.md b/en/star/hr8308.md deleted file mode 100644 index 399e38ddf..000000000 --- a/en/star/hr8308.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Enif (ε Peg) -constellation: Peg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.797210 ---- diff --git a/en/star/hr8316.md b/en/star/hr8316.md deleted file mode 100644 index 4a5f37ee9..000000000 --- a/en/star/hr8316.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Erakis (μ Cep) -constellation: Cep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 13:40:01.462285 ---- -William Herschel named the star "Garnet Star" for its striking, deep red colour - it is one of the reddest stars in the sky, a fact easily verifiable even to the unaided human eye. Even in a binocular or small telescope it provides a nice view. Gradually, when viewed through increasingly larger telescopes, it can take on an orange-red to orange-yellow hue. Its surface temperature is only 3,500 K, while its diameter is 70 times that of the Sun. By comparison, this M spectrum star is actually much brighter than another well-known red giant, Betelgeuse of Orion, equal to at least 174,000 Suns, and has an absolute magnitude of -8.3. We only see it as a faint star in the sky because of its great distance of 2,800 light years. \ No newline at end of file diff --git a/en/star/hr8322.md b/en/star/hr8322.md deleted file mode 100644 index fff2bd10d..000000000 --- a/en/star/hr8322.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Deneb Algedi (δ Cap) -constellation: Cap -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-22 22:06:54.304820 ---- -the brightest star in the constellation. It is an occulting variable star of the Algol type, but its brightness varies only between 2.9mag and 3.1mag, and only over a period of 1.023 days, which is hard to see with the naked eye. It lies at a distance of 38ly. \ No newline at end of file diff --git a/en/star/hr834.md b/en/star/hr834.md deleted file mode 100644 index 09d2f875d..000000000 --- a/en/star/hr834.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Miram (η Per) -constellation: Per -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.593757 ---- diff --git a/en/star/hr8353.md b/en/star/hr8353.md deleted file mode 100644 index a3003b458..000000000 --- a/en/star/hr8353.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: γ Gru -constellation: Gru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.098550 ---- diff --git a/en/star/hr8383.md b/en/star/hr8383.md deleted file mode 100644 index 33bcdd534..000000000 --- a/en/star/hr8383.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: VV Cephei -constellation: Cep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 13:42:13.444553 ---- -red giant, a component of an occultation variable star that varies in apparent brightness from 4.9mag to 5.7mag over a period of 20 years. It was once thought to be the largest known star in the observed part of the universe. It is 2,400 times larger in diameter than the Sun, with an average density of only three millionths that of water. Distance from Earth is 5,000ly. \ No newline at end of file diff --git a/en/star/hr8386.md b/en/star/hr8386.md deleted file mode 100644 index ab55494d6..000000000 --- a/en/star/hr8386.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: η PsA -constellation: PsA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:26:06.396721 ---- -in a 200 mm telescope, this binary system appears as two blue-white disks almost in contact. The components have a brightness of 5.8mag and 6.8mag and are 1.7" apart. \ No newline at end of file diff --git a/en/star/hr8387.md b/en/star/hr8387.md deleted file mode 100644 index d8f13bdc1..000000000 --- a/en/star/hr8387.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: ε Ind -constellation: Ind -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.683060 ---- diff --git a/en/star/hr8417.md b/en/star/hr8417.md deleted file mode 100644 index 31ed1dff9..000000000 --- a/en/star/hr8417.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Al Kurhah (ξ Cep) -constellation: Cep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 13:41:11.869054 ---- -This physical binary is made up of two components of brightness 4.6mag (white) and 6.5mag (yellow-brown) at a separation of 8", which can be resolved in ideal conditions by binoculars with a lens diameter over 6 cm. Their distance from Earth is determined to be 86 light years. It is a peripheral member of the "motion group in Taurus" associated mainly with the open cluster Hyades. \ No newline at end of file diff --git a/en/star/hr8425.md b/en/star/hr8425.md deleted file mode 100644 index 750c2175a..000000000 --- a/en/star/hr8425.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Alnair (α Gruis) -constellation: Gru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.275875 ---- diff --git a/en/star/hr8480.md b/en/star/hr8480.md deleted file mode 100644 index fe1fc727f..000000000 --- a/en/star/hr8480.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 41 Aqr -constellation: Aqr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:17:28.394135 ---- -a binary star consisting of two components with the same brightness of 7.1mag at a distance of 5". In the field of view of a telescope with a lens diameter of about 20 cm, it is a close, equally bright pair of gold and blue components. \ No newline at end of file diff --git a/en/star/hr8486.md b/en/star/hr8486.md deleted file mode 100644 index 6605c978d..000000000 --- a/en/star/hr8486.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: μ Gru -constellation: Gru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.036975 ---- diff --git a/en/star/hr8502.md b/en/star/hr8502.md deleted file mode 100644 index 47b886ad1..000000000 --- a/en/star/hr8502.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: α Tuc -constellation: Tuc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-24 07:40:46.949980 ---- -the brightest star in the constellation has an apparent brightness of 2.91mag and an orange hue. It is 62 light years from Earth. \ No newline at end of file diff --git a/en/star/hr8540.md b/en/star/hr8540.md deleted file mode 100644 index 7db530afa..000000000 --- a/en/star/hr8540.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Tuc -constellation: Tuc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-24 07:42:29.421886 ---- -an easily distinguishable binary star. The main component of brightness 4.8mag has a companion of brightness 9mag at a distance of 7 arc seconds, which we can separate with at least 100 mm telescope. \ No newline at end of file diff --git a/en/star/hr8545.md b/en/star/hr8545.md deleted file mode 100644 index 10f5b3e29..000000000 --- a/en/star/hr8545.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 53 Aqr -constellation: Aqr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:18:03.058151 ---- -multiple stars. At 200 mm, a close pair (3.1") of two yellow suns (6.4mag, 6.6mag), but they are not related at all - just an optical binary. Nearby are two fainter stars, 12.9mag and 13.9mag. \ No newline at end of file diff --git a/en/star/hr8556.md b/en/star/hr8556.md deleted file mode 100644 index 5cdbfd49f..000000000 --- a/en/star/hr8556.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: δ Gru -constellation: Gru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.555683 ---- diff --git a/en/star/hr8559.md b/en/star/hr8559.md deleted file mode 100644 index a86234ea5..000000000 --- a/en/star/hr8559.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Dzeta Aquarii (ζ Aqr) -constellation: Aqr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:16:19.456638 ---- -the famous double star in the Aquarius jug. The two almost equally bright components, 4.3mag and 4.5mag, have a mutual orbital period of 856 years. In 1967, the two stars were only 1.7" apart, but since then their distance has been slowly increasing. In 1985 it was 1.8", but at the beginning of the third millennium we see them as a yellow to white pair about two arc seconds wide, easily resolved even with a small telescope with a 5cm diameter objective. In 2160 their separation will increase to 6". The system is 92 light years away. \ No newline at end of file diff --git a/en/star/hr8571.md b/en/star/hr8571.md deleted file mode 100644 index 8e2cf9cb9..000000000 --- a/en/star/hr8571.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: δ Cephei -constellation: Cep -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 13:38:36.225114 ---- -together with the stars ε (4.19mag) and ζ Cep (3.35mag) form a small triangle. While these two stars are constant, δ Cephei changes its brightness periodically due to pulsations. In fact, a whole group of variable stars - the delta Cepheids - is named after this star. The variability of δ Cephei was discovered in 1784 by 20-year-old John Goodrick, a deaf-mute English amateur astronomer of Dutch origin (he discovered three variable stars, was the first to thoroughly investigate the changes in the brightness of Algol, and explained them correctly at the age of 19; he died two years later at the age of 21). At its brightest, the star reaches 3.48mag, while at its minimum it is 4.37mag, so these changes are easy to observe with the naked eye. Its period is 5.37 days. Cepheids are used by astronomers to estimate distances in space. \ No newline at end of file diff --git a/en/star/hr8576.md b/en/star/hr8576.md deleted file mode 100644 index 6542f0ba3..000000000 --- a/en/star/hr8576.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Fum al Samakah (β PsA) -constellation: PsA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:25:22.381597 ---- - an optical binary star resolved by a good binocular. The main white component of this pair has a brightness of 4.4mag and the bluish guide at 30.3" reaches 7.9mag. \ No newline at end of file diff --git a/en/star/hr86.md b/en/star/hr86.md deleted file mode 100644 index 283744e3c..000000000 --- a/en/star/hr86.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: 42 Psc -constellation: Psc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.335906 ---- diff --git a/en/star/hr8603.md b/en/star/hr8603.md deleted file mode 100644 index e9dbc047b..000000000 --- a/en/star/hr8603.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 8 Lac -constellation: Lac -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-02 13:54:06.509642 ---- -Struve 2922, has so many companions that it could be classified as a poor open cluster rather than just a multiple star. Four close companions, all white or pale blue components lie within 82" of the main star. Another lies 336" WNW. There are also 13-14mag stars in the region. At least a 200mm telescope is required to sufficiently enjoy the appearance. \ No newline at end of file diff --git a/en/star/hr8628.md b/en/star/hr8628.md deleted file mode 100644 index 2feeb8d96..000000000 --- a/en/star/hr8628.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε PsA -constellation: PsA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:24:51.195137 ---- -The companions have a brightness of 5.5mag and 6.5mag, with a separation of 1.6". We need a telescope with an objective lens diameter over 100 mm. \ No newline at end of file diff --git a/en/star/hr8636.md b/en/star/hr8636.md deleted file mode 100644 index 9565efd97..000000000 --- a/en/star/hr8636.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: β Gru -constellation: Gru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.852601 ---- diff --git a/en/star/hr8650.md b/en/star/hr8650.md deleted file mode 100644 index a8e009e10..000000000 --- a/en/star/hr8650.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Matar (η Peg) -constellation: Peg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.955184 ---- diff --git a/en/star/hr8695.md b/en/star/hr8695.md deleted file mode 100644 index f71304bc4..000000000 --- a/en/star/hr8695.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: γ PsA -constellation: PsA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:25:45.986325 ---- -stars with a brightness of 4.5mag and 8.1mag are 4.3" apart. We need a 100 mm telescope to resolve them, mainly because of the difference in brightness of the two components. They lie at a distance of 215ly. \ No newline at end of file diff --git a/en/star/hr8728.md b/en/star/hr8728.md deleted file mode 100644 index 38351ff5a..000000000 --- a/en/star/hr8728.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Fomalhaut (α PsA) -constellation: PsA -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-11 15:24:28.103051 ---- -lies on the doubly elongated Schema-Markab conjunction of the stars of the constellation Pegasus. At 1.2mag, yellow-white Fomalhaut is just 25 light years away and is one of the 20 brightest stars in the sky. Compared to the Sun, it is more than twice the diameter and exceeds our star 16 times in luminosity. \ No newline at end of file diff --git a/en/star/hr8775.md b/en/star/hr8775.md deleted file mode 100644 index 99bd72e24..000000000 --- a/en/star/hr8775.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Scheat (β Peg) -constellation: Peg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.208581 ---- diff --git a/en/star/hr8787.md b/en/star/hr8787.md deleted file mode 100644 index 153c9428e..000000000 --- a/en/star/hr8787.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: θ Gru -constellation: Gru -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.630226 ---- diff --git a/en/star/hr8815.md b/en/star/hr8815.md deleted file mode 100644 index babd81fc3..000000000 --- a/en/star/hr8815.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: 57 Peg -constellation: Peg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.977466 ---- diff --git a/en/star/hr8841.md b/en/star/hr8841.md deleted file mode 100644 index 38add19e9..000000000 --- a/en/star/hr8841.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ψ Aqr -constellation: Aqr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:15:52.398236 ---- -the main star of 4.5mag has a guide of 9.4mag at 49". At 10cm it is a telescope wide, unequally bright pair, consisting of an orange and greenish component that resembles the planet Uranus. Very nice color contrast. \ No newline at end of file diff --git a/en/star/hr8866.md b/en/star/hr8866.md deleted file mode 100644 index d92bce3fe..000000000 --- a/en/star/hr8866.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: 94 Aqr -constellation: Aqr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:17:01.481715 ---- -an easy to resolve and beautiful binary star, consisting of two components of 5.3mag and 7.3mag brightness at 12.7" apart, so even a small telescope is sufficient to resolve it. One has a nice reddish yellow hue and the other a light green hue. \ No newline at end of file diff --git a/en/star/hr887.md b/en/star/hr887.md deleted file mode 100644 index dab307d2b..000000000 --- a/en/star/hr887.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ε Arietis -constellation: Ari -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:31:21.214403 ---- -a double star, white components with almost equal brightness (5.2mag and 5.5mag) at a distance of 1.5". We can separate them sufficiently with 150x magnification using a 200mm telescope during good seeing. \ No newline at end of file diff --git a/en/star/hr897.md b/en/star/hr897.md deleted file mode 100644 index b48be85c4..000000000 --- a/en/star/hr897.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Acamar (θ Eri) -constellation: Eri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.919071 ---- diff --git a/en/star/hr8992.md b/en/star/hr8992.md deleted file mode 100644 index d2e72849d..000000000 --- a/en/star/hr8992.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Aqr -constellation: Aqr -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:18:27.995830 ---- -a variable star whose magnitude can sometimes be as high as 5.8mag, although it is usually much fainter. It shows rapid, unpredictable fluctuations. \ No newline at end of file diff --git a/en/star/hr90.md b/en/star/hr90.md deleted file mode 100644 index 7e024e801..000000000 --- a/en/star/hr90.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: R Andromedae -constellation: And -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-21 17:08:18.291883 ---- -A long-period variable star of the type Mira Ceti, the brightest in this constellation. It lies near a small triangle of stars θ, σ and ρ And. At its maximum of 5.8mag it is at the limit of naked-eye visibility, but in 409.33 days its brightness drops to 14.9mag (changing by 9 magnitudes) and is virtually unobservable with smaller amateur telescopes. The distance is not precisely determined, about 790 light years. \ No newline at end of file diff --git a/en/star/hr9004.md b/en/star/hr9004.md deleted file mode 100644 index 65160bec2..000000000 --- a/en/star/hr9004.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: TX Psc -constellation: Psc -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.769090 ---- diff --git a/en/star/hr9036.md b/en/star/hr9036.md deleted file mode 100644 index 1aeff17c2..000000000 --- a/en/star/hr9036.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: φ1 Peg -constellation: Peg -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.526873 ---- diff --git a/en/star/hr9045.md b/en/star/hr9045.md deleted file mode 100644 index bb6ba2e88..000000000 --- a/en/star/hr9045.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ρ Cas -constellation: Cas -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 10:13:15.269131 ---- -An irregular variable star, like R Coronae Borealis, its brightness varies between 4.1mag and 6.2mag in a cycle that lasts a little less than a year. Suitable comparison stars are σ (4.9mag) and τ Cas (4.87mag). This exceptionally luminous supergiant is 3400 light-years away. It can be seen in the sky near the star β Cas. \ No newline at end of file diff --git a/en/star/hr911.md b/en/star/hr911.md deleted file mode 100644 index e162bdd90..000000000 --- a/en/star/hr911.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: Menkar (α Cet) -constellation: Cet -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-01-23 18:15:57.515936 ---- -an orange giant with an apparent brightness of 2.53mag is 250 light-years away. Nearly 16 arc minutes away to the north lies the star 93 Ceti (5.6mag), visible to the naked eye as an optical guide. \ No newline at end of file diff --git a/en/star/hr936.md b/en/star/hr936.md deleted file mode 100644 index 337baaf6e..000000000 --- a/en/star/hr936.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Algol (β Per) -constellation: Per -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.432910 ---- diff --git a/en/star/hr963.md b/en/star/hr963.md deleted file mode 100644 index 90c2d414c..000000000 --- a/en/star/hr963.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: α For -constellation: For -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.122229 ---- diff --git a/en/star/hr98.md b/en/star/hr98.md deleted file mode 100644 index fb7c044e1..000000000 --- a/en/star/hr98.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: β Hyi -constellation: Hyi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.067463 ---- diff --git a/en/star/hr99.md b/en/star/hr99.md deleted file mode 100644 index ca8bcecee..000000000 --- a/en/star/hr99.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: Ankaa (α Phe) -constellation: Phe -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:57.016066 ---- diff --git a/en/star/hrNone.md b/en/star/hrNone.md deleted file mode 100644 index 9ef64e8c7..000000000 --- a/en/star/hrNone.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: RY Dra -constellation: Dra -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-05 20:22:47.459775 ---- -a variable star with a deep red hue. It is one of the cool carbon stars, notable for the carbon molecules present in its atmosphere. The brightness of the star varies between 9.4mag and 11.4mag over a period of 172 days. In a larger telescope it is always found in the middle of the southeastern side of the isosceles triangle of stars 7, 8 and 9 Draconis. \ No newline at end of file diff --git a/en/star/x_Vel.md b/en/star/x_Vel.md deleted file mode 100644 index 80f740b49..000000000 --- a/en/star/x_Vel.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: x Vel -constellation: Vel -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-08 14:34:28.908673 ---- -a binary star whose 4.3mag and 6.6mag components can be resolved at 52" separation with a binocular. \ No newline at end of file diff --git a/en/star/ι_Tri.md b/en/star/ι_Tri.md deleted file mode 100644 index 65f7edd1a..000000000 --- a/en/star/ι_Tri.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: ι Tri -constellation: Tri -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-04-02 14:53:34.724584 ---- -a binary star whose 5.3mag and 6.9mag brightness components lie 3.9" apart. To resolve the yellow and blue stars we need an 80mm telescope. \ No newline at end of file diff --git a/en/star/π1_UMi.md b/en/star/π1_UMi.md deleted file mode 100644 index 050478143..000000000 --- a/en/star/π1_UMi.md +++ /dev/null @@ -1,9 +0,0 @@ ---- -name: π1 UMi -constellation: UMi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: skybber -updated_date: 2022-02-08 15:23:22.078731 ---- -double star, the main column is yellow (6,6mag) and the companion is white (7,3mag). They lie at a mutual distance of 31.1" and actually orbit each other in 150 years. The star field around it is made up of a string of fairly bright stars, a ring and an arc of three fainter stars. \ No newline at end of file diff --git a/en/star/φ_Hyi.md b/en/star/φ_Hyi.md deleted file mode 100644 index 7338a0203..000000000 --- a/en/star/φ_Hyi.md +++ /dev/null @@ -1,8 +0,0 @@ ---- -name: φ Hyi -constellation: Hyi -created_by: editor.cs -created_date: 2022-01-21 17:00:00 -updated_by: editor.cs -updated_date: 2022-02-11 18:51:56.962460 ----