Английская Википедия:AI Velorum

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AI Velorum is a variable star in the southern constellation of Vela, abbreviated AI Vel. It is a prototype for a class of high amplitude Delta Scuti variables.[1] The apparent visual magnitude of this star fluctuates around 6.56,[2] which is just bright enough to be dimly visible to the naked eye. The distance to AI Vel is approximately 327 light years based on parallax measurements,[3] and it is drifting further away with a radial velocity of about 9 km/s.[4]

The variability of this star was announced by E. Hertzsprung in 1931. He found a period of about Шаблон:Convert,[5] although he later found that period doubtful. In 1937, F. Zagar found irregular variations in the light curve.[6] T. Walraven classified it as an RR Lyrae star in 1952 and suggested it may have two periods that interfered with each other. The primary period was found to be Шаблон:Convert while the secondary is Шаблон:Convert; together their interference creates a beat period of Шаблон:Convert. The height of the maximum was found to be greater than the depth of the minimum, which may be the result of shockwaves that increase light emission.[7]

As an RR Lyrae variable, AI Velorum should be a low mass, evolved star. However, M. Breger in 1977 noted the period and surface gravity showed a match with Delta Scuti stars of the same period. Together with the space velocity, these indicated it is instead a normal, high mass star belonging to the younger population I.[8] By 1985, there was some evidence for an increase in the second period by one part in 105.[9] At least two additional periodicities were identified by Walraven and associates in 1992.[1]

The stellar classification of AI Vel is A9IV/V,[10] matching a slightly evolved star that is moving away from the main sequence. It is 479 million years old and is estimated to have 1.55 times the mass of the Sun.[11] As a Delta Scuti variable, the brightness of the star ranges in magnitude from 6.15 down to 6.76.[12] Evolutionary models published with Gaia Data Release 3 show it to be approaching the end of its main sequence life.[3]

References

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Further reading

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Шаблон:Stars of Vela

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  1. ↑ 1,0 1,1 Ошибка цитирования Неверный тег <ref>; для сносок Walraven_et_al_1992 не указан текст
  2. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Anderson_Francis_2012 не указан текст
  3. ↑ 3,0 3,1 Ошибка цитирования Неверный тег <ref>; для сносок GaiaDR3 не указан текст
  4. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Gontcharov2006 не указан текст
  5. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Hertzsprung_1931 не указан текст
  6. ↑ Ошибка цитирования Неверный тег <ref>; для сносок van_Hoof_1937 не указан текст
  7. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Walraven_1952 не указан текст
  8. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Breger_1977 не указан текст
  9. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Bates_Halliwell_1985 не указан текст
  10. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Houk1978 не указан текст
  11. ↑ Ошибка цитирования Неверный тег <ref>; для сносок David_Hillenbrand_2015 не указан текст
  12. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Samus_et_al_2017 не указан текст
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