Английская Википедия:HD 89890
Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox image Шаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end
HD 89890 is the brightest member of a multiple star system with at least four components,[1] located in the southern constellation of Vela. It is visible to the naked eye with an apparent visual magnitude of 4.50.[2] The annual parallax shift of Шаблон:Val[3] provides a distance estimate of around Шаблон:Convert. It is moving further away from Earth with a heliocentric radial velocity of +10 km/s.[4]
System
The Washington Double Star Catalog lists three visible components for this system. The brightest, component A, is of visual magnitude 4.50. Component B has a magnitude of 7.179,[5] and as of 2000 lies at an angular separation of Шаблон:Val from A, along a position angle (PA) of 102°. Component C is a magnitude 9.125 star[5] at a separation of Шаблон:Val from A at a PA of 191°. The physical link between the stars was described on the basis of their dynamic parallax and mean velocities.[6] The three components A, B and C have Gaia Data Release 2 parallaxes of Шаблон:Val, Шаблон:Val, and Шаблон:Val, respectively.[3]
Properties
Component A has a stellar classification of B3 III, and is categorized as a Be star. It shows photometric variations with multiple periods around 4.6 days and line-profile variations with a period of 2.318 days. The radial velocity of this star is constant.[1] It has 10[7] times the Sun's radius and shines with 3,082[4] times the Sun's luminosity from its photosphere at an effective temperature of Шаблон:Val.[7]
The component B shows a variation in spectra consistent with being a double-lined spectroscopic binary. The brighter member (Ba) is a silicon star with a class of A0 IVpSi, while the fainter component (Bb) is of type A2. Component C has a class of K0 III, indicating it is an evolved giant star. The measured effective temperature of C is 5,500 K. The fact that component A most likely shares a common origin with C suggests that the former is much older than expected, and may actually be a blue straggler formed from the merger of a close binary. This could have been caused by the gravitational influence of an unseen companion of A.[1]
References
- ↑ 1,0 1,1 1,2 Ошибка цитирования Неверный тег
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<ref>; для сносокGaiaDR2не указан текст - ↑ 4,0 4,1 Ошибка цитирования Неверный тег
<ref>; для сносокAnderson2012не указан текст - ↑ 5,0 5,1 Ошибка цитирования Неверный тег
<ref>; для сносокtycho2не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокWDSC2014не указан текст - ↑ 7,0 7,1 Ошибка цитирования Неверный тег
<ref>; для сносокArcos2018не указан текст
- Английская Википедия
- B-type giants
- Be stars
- Blue stragglers
- Multiple star systems
- Vela (constellation)
- Bayer objects
- Durchmusterung objects
- Henry Draper Catalogue objects
- Bright Star Catalogue objects
- Objects with variable star designations
- Hipparcos objects
- Ap stars
- A-type subgiants
- A-type main-sequence stars
- K-type giants
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- Страницы с телепортом
- Википедия
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- Статья из Английской Википедии
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