Английская Википедия:HD 4113

Материал из Онлайн справочника
Версия от 03:23, 18 марта 2024; EducationBot (обсуждение | вклад) (Новая страница: «{{Английская Википедия/Панель перехода}} {{Short description|Binary star system in the constellation of Sculptor}} {{Starbox begin}} {{Starbox observe 2s | epoch = J2000.0 | constell = Sculptor | component1 = HD 4113 A | ra1 = {{RA|00|43|12.59559}}<ref name="Gaia DR3 A"/> | dec1 = {{DEC|-37|58|57.4777}}<ref name="Gaia DR3 A"/> | appmag_v1 = {{Val|7.880|0.013}}<ref...»)
(разн.) ← Предыдущая версия | Текущая версия (разн.) | Следующая версия → (разн.)
Перейти к навигацииПерейти к поиску

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 4113 is a dual star system in the southern constellation of Sculptor. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 7.88.[1] The distance to this star, as estimated by parallax measurements, is 137 light years.[2] It is receding away from the Sun with a radial velocity of +5 km/s.[2]

The primary member of this system, component A, is a Sun-like G-type main-sequence star with a stellar classification of G5V.[1] Estimates of its age are five[1] to seven[3] billion years old, and it is spinning with a leisurely projected rotational velocity of 2.3 km/s.[1] The star is metal rich, with nearly the same mass,[3] radius, and luminosity[4] as the Sun.

Orbiting this star is a giant planet and a brown dwarf (HD 4113 C); the latter has been directly imaged. It also has a co-moving stellar companion, designated component B, which is a red dwarf with a class of M0–1V at an angular separation of Шаблон:Val. This angle is equivalent to a projected separation of Шаблон:Val.[1]

The most recent parameters for HD 4113 C as of 2022 come from a combination of data from radial velocity, astrometry, and imaging, showing that it is about 52 times the mass of Jupiter, and on an eccentric orbit with a semi-major axis of about 50.4 AU and an orbital period of about 348 years.[5]

Planetary system

On 26 October 2007, Tamuz et al. used the radial velocity method to find a planet with a minimum mass one and half times that of Jupiter orbiting at 1.28 AU away from HD 4113 A. The planet's orbit is highly eccentric.[6]

Шаблон:OrbitboxPlanet begin Шаблон:OrbitboxPlanet Шаблон:Orbitbox end

See also

References

Шаблон:Reflist

External links

Шаблон:Sky

Шаблон:Stars of Sculptor

Партнерские ресурсы
Криптовалюты
Магазины
Хостинг
Разное

  1. ↑ 1,0 1,1 1,2 1,3 1,4 Ошибка цитирования Неверный тег <ref>; для сносок Cheetham2018 не указан текст
  2. ↑ 2,0 2,1 Ошибка цитирования Неверный тег <ref>; для сносок Gaia DR3 A не указан текст
  3. ↑ 3,0 3,1 Ошибка цитирования Неверный тег <ref>; для сносок AguileraGómez2018 не указан текст
  4. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Gaia DR2 не указан текст
  5. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Feng2022 не указан текст
  6. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Tamuz2008 не указан текст
Источник — http://wikihandbk.com/ruwiki/index.php?title=Английская_Википедия:HD_4113&oldid=15086788