Английская Википедия:HD 126614
Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox observe 2s Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox orbit Шаблон:Starbox detail Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end
HD 126614 is a trinary star[1] system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81,[2] it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements,[3] but is drifting closer with a radial velocity of −33 km/s.[4]
Stellar system
HD 126614 A
The primary is a late G-type star with a stellar classification of G8IV.[5] It is a super metal-rich star; among the most metal-rich stars currently known.[6] This is most likely an evolving subgiant star, but the very high metallicity makes comparisons to standard spectral types difficult.[7]
HD 126614 C
In 2010, a close stellar companion was resolved and designated component C. This object is a faint red dwarf at an angular separation of Шаблон:Val, which corresponds to a projected physical separation of Шаблон:Val.[7] More recent observations using radial velocity and astrometry have refined the parameters of HD 126614 C. It has an orbital period of about 60 years, with a smaller semi-major axis of 15 AU and a very low mass of Шаблон:Jupiter mass.[8] This mass is very near the mass limit allowed for hydrogen fusion.
HD 126614 B
The outer companion, designated LP 680-57, was first reported in 1960 with the W. J. Luyten proper motion catalog.[9] It is a magnitude 17.0 red dwarf with a class of M5.5,[10] located at an angular separation of Шаблон:Val from the primary along a position angle of 299°, as of 2015.[9] They have a physical projected separation of Шаблон:Val.[10] The common proper motion of the system has been confirmed, indicating that they are gravitationally bound.[7] Many multiple star catalogues still refer to this companion as component B, as it was known prior to the discovery of the closer companion.[9]
Planetary system
A Doppler search for giant planets begun in 1997 at the Keck Observatory provided an 11 year baseline for detecting periodicity in the primary star's radial velocity data. In 2010, a Jovian companion was announced with an orbital period of Шаблон:Convert.[11] In 2022, the inclination and true mass of HD 126614 Ab were measured via astrometry.[8]
Шаблон:OrbitboxPlanet begin Шаблон:OrbitboxPlanet Шаблон:Orbitbox end
See also
References
- ↑ Ошибка цитирования Неверный тег
<ref>; для сносокBusetti_et_al_2018не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокAnderson_Francis_2012не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокGaia DR3 Aне указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокSoubiran_et_al_2018не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокHouk_Swift_1999не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокCastro_et_al_1997не указан текст - ↑ 7,0 7,1 7,2 Ошибка цитирования Неверный тег
<ref>; для сносокLodieu_et_al_2014не указан текст - ↑ 8,0 8,1 Ошибка цитирования Неверный тег
<ref>; для сносокFeng2022не указан текст - ↑ 9,0 9,1 9,2 Ошибка цитирования Неверный тег
<ref>; для сносокMason_et_al_2014не указан текст - ↑ 10,0 10,1 Ошибка цитирования Неверный тег
<ref>; для сносокDeacon2014не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокHoward2010не указан текст
- Английская Википедия
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