From f9d67faf061ac7f8cfadbe3faa0d266269edf098 Mon Sep 17 00:00:00 2001 From: Vladimir Dvorak Date: Fri, 11 Feb 2022 19:43:51 +0100 Subject: [PATCH] Triad fix --- en/star/R_Ara.md | 2 +- en/star/V_Sge.md | 2 +- en/star/hr1983.md | 2 +- en/star/hr2061.md | 2 +- en/star/hr2742.md | 2 +- en/star/hr3789.md | 2 +- en/star/hr4104.md | 2 +- en/star/hr4234.md | 2 +- en/star/hr4898.md | 2 +- en/star/hr5531.md | 2 +- en/star/hr5894.md | 2 +- en/star/hr6107.md | 2 +- en/star/hr6923.md | 2 +- en/star/hr7066.md | 2 +- en/star/hr7139.md | 2 +- en/star/hr7141.md | 2 +- 16 files changed, 16 insertions(+), 16 deletions(-) diff --git a/en/star/R_Ara.md b/en/star/R_Ara.md index 048432d12..8e2d2ee0a 100644 --- a/en/star/R_Ara.md +++ b/en/star/R_Ara.md @@ -6,4 +6,4 @@ 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 triad along with the stars ζ and η Ara. \ No newline at end of file +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/V_Sge.md b/en/star/V_Sge.md index 7fb59e1de..b270d88ff 100644 --- a/en/star/V_Sge.md +++ b/en/star/V_Sge.md @@ -6,4 +6,4 @@ 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 triad. Almost every night it is differently bright, changing magnitude erratically from 8.6 to 13.9. \ No newline at end of file +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/hr1983.md b/en/star/hr1983.md index fd129f1f7..89840a382 100644 --- a/en/star/hr1983.md +++ b/en/star/hr1983.md @@ -6,4 +6,4 @@ 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 triad, 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 +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/hr2061.md b/en/star/hr2061.md index 13da46669..0ff969fbd 100644 --- a/en/star/hr2061.md +++ b/en/star/hr2061.md @@ -6,4 +6,4 @@ 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 triad. 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 +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/hr2742.md b/en/star/hr2742.md index ff545dc88..6474df4f3 100644 --- a/en/star/hr2742.md +++ b/en/star/hr2742.md @@ -6,4 +6,4 @@ 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 triad. 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 +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/hr3789.md b/en/star/hr3789.md index 3f3dfe64c..77095b05f 100644 --- a/en/star/hr3789.md +++ b/en/star/hr3789.md @@ -6,4 +6,4 @@ 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 triad 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 +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/hr4104.md b/en/star/hr4104.md index d9b6c6084..30dab3bd1 100644 --- a/en/star/hr4104.md +++ b/en/star/hr4104.md @@ -6,4 +6,4 @@ 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 triad, 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 +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/hr4234.md b/en/star/hr4234.md index 8b64dfebc..7a52d0fea 100644 --- a/en/star/hr4234.md +++ b/en/star/hr4234.md @@ -6,4 +6,4 @@ 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 triad 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 +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/hr4898.md b/en/star/hr4898.md index 61490b00d..3c90848b1 100644 --- a/en/star/hr4898.md +++ b/en/star/hr4898.md @@ -6,4 +6,4 @@ 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 triad 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 +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/hr5531.md b/en/star/hr5531.md index ca3e0511e..5b74ec61a 100644 --- a/en/star/hr5531.md +++ b/en/star/hr5531.md @@ -6,4 +6,4 @@ 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 triad 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 +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/hr5894.md b/en/star/hr5894.md index 81e98c574..de06aab00 100644 --- a/en/star/hr5894.md +++ b/en/star/hr5894.md @@ -6,4 +6,4 @@ 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 triad 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 +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/hr6107.md b/en/star/hr6107.md index a7155a7db..c91b8fd95 100644 --- a/en/star/hr6107.md +++ b/en/star/hr6107.md @@ -6,4 +6,4 @@ 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 triad 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 +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/hr6923.md b/en/star/hr6923.md index 17224bc4f..f7c759e06 100644 --- a/en/star/hr6923.md +++ b/en/star/hr6923.md @@ -6,4 +6,4 @@ 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 triad 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 +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/hr7066.md b/en/star/hr7066.md index 8b46b122f..7c27bab0a 100644 --- a/en/star/hr7066.md +++ b/en/star/hr7066.md @@ -6,4 +6,4 @@ 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 triad, 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 +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/hr7139.md b/en/star/hr7139.md index edbd19000..405de82b7 100644 --- a/en/star/hr7139.md +++ b/en/star/hr7139.md @@ -6,4 +6,4 @@ 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 triad. \ No newline at end of file +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 index e3dd68a64..cfbc94481 100644 --- a/en/star/hr7141.md +++ b/en/star/hr7141.md @@ -6,4 +6,4 @@ 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 triad 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 +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