V638 Андромеды

V638 Андромеды
Звезда
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Наблюдательные данные
(Эпоха J2000.0)
Прямое восхождение 23ч 19м 50,53с[1]
Склонение +44° 07′ 33,45″[1]
Расстояние 285,1115 ± 2,6175 пк[1]
Видимая звёздная величина (V) 11,37 ± 0,09[2]
Созвездие Андромеда
Астрометрия
Лучевая скорость (Rv) 9,4 ± 17,77 км/с[1]
Собственное движение
 • прямое восхождение 32,364 ± 0,048 mas/год[1]
 • склонение −1,653 ± 0,04 mas/год[1]
Параллакс (π) 3,5074 ± 0,0322 mas[1]
Спектральные характеристики
Показатель цвета
 • B−V 0,56
Переменность W Большой Медведицы[3][4][…]
Коды в каталогах
TYC 3229-48-1, GSC 03229-00048, 2MASS J23195051+4407333, NSVS 3552946, Gaia DR1 1937048564237342080, Gaia DR2 1937048568535232384, V638 And и TIC 173795590
Информация в базах данных
SIMBAD NSVS 3552946
Логотип Викиданных Информация в Викиданных ?

V638 Андромеды (лат. V638 Andromedae) — двойная затменная переменная звезда типа W Большой Медведицы (EW) в созвездии Андромеды на расстоянии приблизительно 930 световых лет (около 285 парсеков) от Солнца. Видимая звёздная величина звезды — от +11,92m до +11,52m[5]. Орбитальный период — около 0,3327 суток (7,985 часов)[6].

Характеристики

Первый компонент — жёлтый карлик спектрального класса G. Масса — около 1,058 солнечной, радиус — около 1,209 солнечного, светимость — около 1,715 солнечной. Эффективная температура — около 5400 K[1].

Второй компонент — жёлтый карлик спектрального класса G.

Планетная система

В 2018 году учёными, анализирующими данные проекта TESS, у звезды обнаружена планета[7].

Планета
 Масса
(MG) 		Радиус
(RG) 		Период обращения
(суток) 		Большая полуось
орбиты (а.е.) 		Эксцентриситет
орбиты
TIC 173795590 b - 3,573 7,487532 - 0,085426

Примечания

  1. ↑ 1 2 3 4 5 6 7 8 Gaia Data Release 2 (англ.) / Data Processing and Analysis Consortium, European Space Agency — 2018.
  2. ↑ Høg E., Fabricius C., Makarov V. V., Urban S., Corbin T., Wycoff G., Bastian U., Schwekendiek P., Wicenec A. The Tycho-2 catalogue of the 2.5 million brightest stars (англ.) // Astronomy and Astrophysics / T. Forveille — EDP Sciences, 2000. — Vol. 355. — P. L27—L30. — ISSN 0004-6361; 0365-0138; 1432-0746; 1286-4846
  3. ↑ Hoffman D. I., Harrison T. E., McNamara B. J. Automated variable star classification using the Northern Sky Variability Survey (англ.) // The Astronomical Journal / J. G. III, E. Vishniac — New York City: IOP Publishing, AAS, University of Chicago Press, AIP, 2009. — Vol. 138, Iss. 2. — P. 466–477. — ISSN 0004-6256; 1538-3881 — doi:10.1088/0004-6256/138/2/466
  4. ↑ N. N. Samus’, Kazarovets E. V., Durlevich O. V., Kireeva N. N., Pastukhova E. N. General catalogue of variable stars: Version GCVS 5.1 (англ.) // Astronomy Reports / D. Bisikalo — MAIK Nauka/Interperiodica, Springer Science+Business Media, 2017. — Vol. 61, Iss. 1. — P. 80–88. — ISSN 1063-7729; 1562-6881; 0004-6299 — doi:10.1134/S1063772917010085
  5. ↑ V638 And, database entry, Combined General Catalog of Variable Stars (GCVS5.1, 2017 Ed.), N. N. Samus, O. V. Durlevich, et al., CDS ID II/250 Архивная копия от 1 июля 2015 на Wayback Machine Accessed online 2021-03-07.
  6. ↑ Kreiner J. M. Up-to-date linear elements of eclipsing binaries (англ.) // Acta Astronomica / M. Kubiak — Copernicus Foundation for Polish Astronomy, 2004. — Vol. 54. — P. 207–210. — ISSN 0001-5237
  7. ↑ Barclay T., Pepper J., Quintana E. V. A Revised Exoplanet Yield from the Transiting Exoplanet Survey Satellite (TESS) (англ.) // The Astrophysical Journal: Supplement Series — AAS, 2018. — Vol. 239, Iss. 1. — P. 2. — ISSN 0067-0049; 1538-4365 — doi:10.3847/1538-4365/AAE3E9 — arXiv:1804.05050

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