V817 Геркулеса

V817 Геркулеса
Звезда
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Наблюдательные данные
(Эпоха J2000.0)
Прямое восхождение 17ч 08м 47,69с[1]
Склонение +42° 41′ 0,56″[1]
Расстояние 713,318 ± 26,357 пк[1]
Созвездие Геркулес
Астрометрия
Собственное движение
 • прямое восхождение −9,751 ± 0,061 mas/год[1]
 • склонение 20,137 ± 0,068 mas/год[1]
Параллакс (π) 1,4019 ± 0,0518 mas[1]
Спектральные характеристики
Спектральный класс PG1159[2][3][…]
Физические характеристики
Температура 0 К[2]
Коды в каталогах
SDSS J170847.68+424100.7, SDSS J170847.69+424100.7, SDSS J170847.68+424100.6, Gaia DR2 1355161726346266112, V817 Her, SDSS J170847.68+424100.8 и Gaia DR3 1355161726346266112
Информация в базах данных
SIMBAD PG 1707+427
Логотип Викиданных Информация в Викиданных ?

V817 Геркулеса (лат. V817 Herculis) — одиночная переменная звезда в созвездии Геркулеса на расстоянии приблизительно 2512 световых лет (около 770 парсек) от Солнца. Видимая звёздная величина звезды — от +16,32m до +16,18m[4].

Открыта Говардом Бондом в 1984 году[5]*[6].

Характеристики

V817 Геркулеса — белый карлик, пульсирующая переменная звезда типа GW Девы (ZZO)[4][7][8] спектрального класса DOZ1[9]. Масса — около 0,542 солнечной, радиус — около 0,0209 солнечного, светимость — около 25,119 солнечной[5]*. Эффективная температура — около 85000 K[10]*.

Примечания

  1. ↑ 1 2 3 4 5 6 Gaia Early Data Release 3 (англ.) / Data Processing and Analysis Consortium, European Space Agency — 2020.
  2. ↑ 1 2 Kleinman S. J., Kepler S. O., Koester D., Peçanha V., Nitta A., Costa J. E. S., Krzesinski J., Pelisoli I., Yip C., Harris H. C. et al. SDSS DR7 white dwarf catalog (англ.) // The Astrophysical Journal: Supplement Series — AAS, 2012. — Vol. 204, Iss. 1. — P. 5. — ISSN 0067-0049; 1538-4365 — doi:10.1088/0067-0049/204/1/5 — arXiv:1212.1222
  3. ↑ Green R. F., Schmidt M., Liebert J. The Palomar-Green catalog of ultraviolet-excess stellar objects (англ.) // The Astrophysical Journal: Supplement Series — AAS, 1986. — Vol. 61. — P. 305–352. — ISSN 0067-0049; 1538-4365 — doi:10.1086/191115
  4. ↑ 1 2 V817 Her, 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 2022-12-21
  5. ↑ 1 2 Córsico A. H., Althaus L. G., Bertolami M. M. M., García-Berro E. Asteroseismology of hot pre-white dwarf stars: the case of the DOV stars PG 2131+066 and PG 1707+427, and the PNNV star NGC 1501 (англ.) // Astronomy and Astrophysics / T. Forveille — EDP Sciences, 2009. — Vol. 499, Iss. 1. — P. 257–266. — ISSN 0004-6361; 0365-0138; 1432-0746; 1286-4846 — doi:10.1051/0004-6361/200810727 — arXiv:0903.3628
  6. ↑ Bond H. E., Grauer A. D., Green R. F., Liebert J. W. Two new extremely hot pulsating white dwarfs (англ.) // The Astrophysical Journal Letters — United Kingdom: IOP Publishing, 1984. — Vol. 279. — P. 751–757. — ISSN 2041-8205; 2041-8213 — doi:10.1086/161943
  7. ↑ 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
  8. ↑ Calcaferro L. M., Corsico A. H., Althaus L. G. Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47 (англ.) // Astronomy and Astrophysics / T. Forveille — EDP Sciences, 2016. — Vol. 589. — P. 40–40. — ISSN 0004-6361; 0365-0138; 1432-0746; 1286-4846 — doi:10.1051/0004-6361/201527996 — arXiv:1602.06355
  9. ↑ McCook G. P., Sion E. M. A Catalogue of Spectroscopically Identified White Dwarfs — 2016. — Т. 1. — С. 2035.
  10. ↑ Hoyer D., Rauch T., Werner K., Kruk J. W. Search for trans-iron elements in hot, helium-rich white dwarfs with the HST Cosmic Origins Spectrograph (англ.) // Astronomy and Astrophysics / T. Forveille — EDP Sciences, 2018. — Vol. 612. — P. 62–62. — ISSN 0004-6361; 0365-0138; 1432-0746; 1286-4846 — doi:10.1051/0004-6361/201732401 — arXiv:1801.02414

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