Английская Википедия:BE Ursae Majoris

Материал из Онлайн справочника
Перейти к навигацииПерейти к поиску

Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox imageШаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end

BE Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated BE UMa. The two components are an unusual M-class dwarf star and a subdwarf O star, borderline white dwarf. It is classified as a detached Algol variable and ranges in brightness from an apparent visual magnitude of 14.8 down to 17.8.[1] This is too faint to be visible to the naked eye. The distance to this system is approximately 4,600 light years based on parallax measurements.[2]

The variability of SVS 1424 was announced in 1964 by N. E. Kurochkin from Sternberg,[3] and was found to have a period of 2.291 days while ranging in brightness from magnitude 14.1 down to 15.6.[4] After being assigned the variable star designation BE UMa, it was discovered to be a source of hot ultraviolet emission with a helium-rich spectrum by D. H. Ferguson and associates in 1981.[5] B. Margon and associates found variability of spectral features on a time scale as low as a few hours. They interpreted this as a detached binary system consisting of a compact, high temperature white dwarf and a cool red dwarf star. The outer layers of the cooler star are being ionized by radiation from the hotter component,[6] and the changing orientation of this heated region over the course of an orbit is creating a sinusoidal variability of about 1.5 magnitudes.[7]

In 1982, a deep eclipse was discovered in the light curve by H. Ando and associates. This put a strong limit on the possible models for the system, which indicated that the compact component is a hot O-type subdwarf.[8] D. Crampton and associates in 1983 found that the temperature and radius of the cool component suggested that it is an evolved subgiant star. At present, no mass transfer is taking place, but the system appears to be evolving into a cataclysmic variable as the subdwarf cools to become a normal white dwarf.[7]

In 1995, J. Liebert and associates discovered that the system is surrounded by a planetary nebula with a diameter of Шаблон:Val, which was likely shed when the present day subdwarf was leaving the asymptotic giant branch stage. The two components would have shared a common envelope as little as 10,000 years ago. As a result, rather than being a subgiant, the cool component has not yet reached the thermal equilibrium of a late dwarf star.[9] The pair have a circular orbit with a period of 2.2911658 days and a separation of Шаблон:Val. The orbital plane is inclined at an angle of Шаблон:Val to the line of sight from the Earth.[10]

References

Шаблон:Reflist

Further reading

Шаблон:Div col

Шаблон:Div col end

Шаблон:Stars of Ursa Major

Партнерские ресурсы
Криптовалюты
Магазины
Хостинг
Разное

  1. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Samus_et_al_2017 не указан текст
  2. ↑ Ошибка цитирования Неверный тег <ref>; для сносок GaiaEDR3 не указан текст
  3. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Kurochkin_1964 не указан текст
  4. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Kurochkin_1971 не указан текст
  5. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Ferguson_et_al_1981 не указан текст
  6. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Margon_et_al_1981 не указан текст
  7. ↑ 7,0 7,1 Ошибка цитирования Неверный тег <ref>; для сносок Crampton_et_al_1983 не указан текст
  8. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Ando_et_al_1982 не указан текст
  9. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Liebert_et_al_1995 не указан текст
  10. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Ferguson_et_al_1999 не указан текст
Источник — http://wikihandbk.com/ruwiki/index.php?title=Английская_Википедия:BE_Ursae_Majoris&oldid=13349337