Английская Википедия:HD 154088
Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end
HD 154088 is a seventh magnitude metal-rich K-type main sequence star that lies approximately 58 light-years away in the constellation of Ophiuchus. The star is orbited by a hot Super-Earth.
Properties
HD 154088 is a modestly bright star that lies at the bottom of Ophiuchus, near to the border with Scorpius and near to the plane of the Milky Way. The star was recognised as a high proper motion star during the last century, and early Earth-based parallax measurements such as that of the Gliese Catalogue of Nearby Stars indicated a distance of about 50 light-years.
The star has a spectral type of K0V, indicating that it is a main sequence star that is about 350 degrees cooler than the Sun. On the Hertzsprung-Russell diagram (left), the star lies slightly above the main sequence. This is because the star is very metal-rich; with an Fe/H of 0.3 dex the star has about twice the solar abundance of iron, which makes HD 154088 fall into the somewhat vague group of super metal-rich (SMR) stars. The giant planet occurrence rate of Fe/H = 0.3 stars is on the order of 30%, but HD 154088 is not currently known to host any giant planets.
HD 154088 has a pronounced magnetic field.[1] It also has a magnetic cycle similar to the Sun,[2] though its length is not well constrained.
The survey in 2015 have ruled out the existence of any additional stellar companions at projected distances from 8 to 119 astronomical units.[3]
Planetary system
A planet orbiting HD 154088 discovered with the HARPS spectrograph was announced in September 2011. With a minimum mass of 6 Earth masses, the companion falls into the regime of Super-Earths.
Шаблон:OrbitboxPlanet begin Шаблон:OrbitboxPlanet Шаблон:Orbitbox end
HD 154088 is also being observed under the Keck Eta-Earth radial velocity survey.[4] HD 154088 b is a close match for planet candidate 1 (orbital period = 18.1 days, minimum mass = 6.5 M🜨), so they may be the same detection. The planet existence was finally confirmed in 2021.[5]
References
- ↑ Ошибка цитирования Неверный тег
<ref>; для сносокFossati2013не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокLovis2011не указан текст - ↑ Шаблон:Cite journal
- ↑ Ошибка цитирования Неверный тег
<ref>; для сносокHoward2010не указан текст - ↑ Шаблон:Citation
- Английская Википедия
- Страницы с неработающими файловыми ссылками
- Ophiuchus
- Durchmusterung objects
- Henry Draper Catalogue objects
- Hipparcos objects
- Gliese and GJ objects
- K-type main-sequence stars
- Страницы, где используется шаблон "Навигационная таблица/Телепорт"
- Страницы с телепортом
- Википедия
- Статья из Википедии
- Статья из Английской Википедии
- Страницы с ошибками в примечаниях
