Английская Википедия:Iota Cassiopeiae
Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox image Шаблон:Starbox observe 3s Шаблон:Starbox character Шаблон:Starbox character Шаблон:Starbox character Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox orbit Шаблон:Starbox orbit Шаблон:Starbox detail Шаблон:Starbox detail Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end Iota Cassiopeiae (ι Cas, ι Cassiopeiae) is a star system in the constellation Cassiopeia. The system has a combined apparent magnitude of 4.53,Шаблон:Cn making it visible to the naked eye. Based on its parallax, it is located about 133 light-years (41 parsecs) from Earth.[1]
Components
Iota Cassiopeiae is known to be a quintuple star system. The brightest star system, ι Cassiopeiae A, contains a white-colored A-type main-sequence star with a mean apparent magnitude of +4.61.[3] The primary is itself a tighter binary star system. The two stars were resolved by adaptive optics.Шаблон:Cn These are designated Aa and Ab (although confusingly they may also be labeled as A and Aa, respectively).Шаблон:Cn The primary is classified as an Alpha2 Canum Venaticorum-type variable star and the brightness of the system varies from magnitude +4.45 to +4.53 with a period of 1.74 days,[4] because of its magnetic field.[5] The fainter companion is a G-type star with a mass of Шаблон:Solar mass.[6] The orbital period of the system is about 49 years.[6]
ι Cassiopeiae B is a yellow-white F-type main sequence dwarf with an apparent magnitude of +6.87.[3] It orbits around ι Cassiopeiae A approximately every 2,400 years with a semi-major axis of around 6.5 arcseconds, but the orbit is not very well constrained.[6] This object may be causing Kozai–Lidov cycles in the inner orbital pair.[6]
ι Cassiopeiae C is itself another binary, designated Ca and Cb,[6] or just C and c.[7] It comprises two stars, a K-type star and an M-type star.[7] It is currently at an angular distance of about 7 arcseconds from the AB pair.[8] Since the semimajor axis of the AB orbit is about 6.5 arcseconds, the true semimajor axis of C's orbit around them is thought to be significantly larger than 7 arcseconds.[6]
References
Шаблон:Var-star-stub
Шаблон:Multi-star-stub
- ↑ Ошибка цитирования Неверный тег
<ref>; для сносокHIPне указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокMASTне указан текст - ↑ 3,0 3,1 Ошибка цитирования Неверный тег
<ref>; для сносокTYC2не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокGCVSне указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокAuriereне указан текст - ↑ 6,0 6,1 6,2 6,3 6,4 6,5 Ошибка цитирования Неверный тег
<ref>; для сносокTokovinin 2021не указан текст - ↑ 7,0 7,1 Ошибка цитирования Неверный тег
<ref>; для сносокChristouне указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокMSCне указан текст
- Английская Википедия
- Страницы с неработающими файловыми ссылками
- Alpha2 Canum Venaticorum variables
- Bayer objects
- Cassiopeia (constellation)
- Multiple star systems
- Spectroscopic binaries
- A-type main-sequence stars
- F-type main-sequence stars
- G-type main-sequence stars
- Bright Star Catalogue objects
- Henry Draper Catalogue objects
- Hipparcos objects
- Durchmusterung objects
- Ap stars
- Страницы, где используется шаблон "Навигационная таблица/Телепорт"
- Страницы с телепортом
- Википедия
- Статья из Википедии
- Статья из Английской Википедии
- Страницы с ошибками в примечаниях
