Английская Википедия:HD 109271
Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox relpos Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end
HD 109271 is a wide binary star system in the constellation of Virgo. The brighter member of the binary has a pair of orbiting exoplanets. With an apparent visual magnitude of 8.05,[1] it cannot be seen with the naked eye. Parallax measurements made by Gaia put the star at a distance of Шаблон:Convert away from the Sun, but it is drifting closer with a radial velocity of −5 km/s.[2] The system shows a high proper motion, traversing the celestial sphere at an angular rate of Шаблон:Val.[3]
The primary component is an ordinary G-type main-sequence star with a stellar classification of G5 V. It is a much older star than the Sun with an age of about 7.3 billion years, and is spinning with a projected rotational velocity of 2.7 km/s.[1] This star has 7% more mass than the Sun and a 30% greater girth.[4] The abundance of iron, a measure of the star's metallicity, is similar but slightly higher than in the Sun.[1] It is radiating 1.65[4] times the luminosity of the Sun from its photosphere at an effective temperature of around 5,783 K.[1]
In 2020, a white dwarf companion of Шаблон:Solar mass was found orbiting the primary at an angular separation of Шаблон:Val along a position angle of 267°. At the distance of this system, this corresponds to a projected separation of Шаблон:Val. That is, they are physically separated by at least this distance. Additional stellar companions are ruled out down to a separation of Шаблон:Val from the primary.[5]
Planetary system
From 2003 to 2012, the star was under observance from the High Accuracy Radial Velocity Planet Searcher (HARPS).[1] In 2012, two eccentric hot Neptune-mass planets were deduced by radial velocity. They were published in January 2013. These are close to a 1:4 resonance, so the system is similar to HD 69830. A third Neptune in the Venus zone was hypothesised from the data. These planets managed to survive the post main-sequence epoch of the companion star, when it shed much of its original mass.[5]
Шаблон:OrbitboxPlanet begin Шаблон:OrbitboxPlanet Шаблон:OrbitboxPlanet Шаблон:OrbitboxPlanet hypothetical Шаблон:Orbitbox end
References
- ↑ 1,0 1,1 1,2 1,3 1,4 Ошибка цитирования Неверный тег
<ref>; для сносокHARPSне указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокSoubiran_et_al_2018не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокLuyten1995не указан текст - ↑ 4,0 4,1 Ошибка цитирования Неверный тег
<ref>; для сносокJohns_et_al_2018не указан текст - ↑ 5,0 5,1 Ошибка цитирования Неверный тег
<ref>; для сносокGinski_et_al_2021не указан текст
- Английская Википедия
- G-type main-sequence stars
- White dwarfs
- Planetary systems with two confirmed planets
- Binary stars
- Virgo (constellation)
- Durchmusterung objects
- Henry Draper Catalogue objects
- Hipparcos objects
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