Английская Википедия:CV Serpentis

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Шаблон:Starbox begin Шаблон:Starbox image Шаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox orbit Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end

CV Serpentis is a binary star system in the equatorial constellation of Serpens. It is a detached eclipsing binary with an orbital period of 29.7 days.[1] The system includes a Wolf–Rayet (WR) star with the identifier WR 113. The system is located at a distance of approximately 6,700 light years from the Sun based on parallax measurements.[2] It is a member of the Serpens OB2 association of co-moving stars.[3]

In 1892, this star was found to be an object of interest based on photographs of its peculiar stellar spectra taken from the Boyden Station in Arequipa, Peru.[4] It was determined to be a carbon-type Wolf–Rayet (WR) star and in 1945 was found to be a spectroscopic binary system by W. A. Hiltner.[5] This system was reported to be an eclipsing binary by S. Gaposchkin in 1949,[6] who found a decrease in brightness of 0.14 magnitude during the first eclipse and 0.08 in the second. R. M. Hjellming and W. A. Hiltner in 1963 measured a much deeper primary eclipse with a decrease of about 0.55 magnitude,[7] then in 1970 K. Stępień saw no evidence of eclipsing.[8] L. V. Kuhi and F. Schweizer confirmed this latter result, hypothesizing that it is the result of a changing Wolf-Rayet envelope.[9]

This is a double-lined spectroscopic binary system in a near circular orbit, meaning that the spectra of both components is visible.[10] The companion of the WR star is a massive OB star with a stellar classification of O8-9IV.[10] A nebulous double-shell centered on CV Ser was discovered in 1984, spanning angular diameters of Шаблон:Val and Шаблон:Val. The diffuse outer ring is incomplete, spanning a radius of Шаблон:Val at an approximate distance of two kiloparsecs.[11] Variations in the system's light curve continued to be observed, suggesting changes in the outflow from the Wolf-Rayet star.[12] An emission feature in the spectrum of the system was interpreted as a region between the two stars where their stellar winds are colliding,[13] forming a shock region of plasma.[10]

The system is expected to evolve into a binary with the OB-star and an Шаблон:Solar mass black hole following a failed supernova where the WR star collapses with little or no visible explosion.[14] The OB star is observed to be rotating rapidly at between 310 and Шаблон:Val using spectral lines of neutral helium. Observations using ionized helium absorption lines show a lower velocity, interpreted as showing an oblate shape with gravity darkening causing lower temperatures at the equator.[15]

Speckle interferometry has found a companion star Шаблон:Val from the bright primary and eight magnitudes fainter. The projected separation of Шаблон:Val is much larger than the maximum possible Шаблон:Val separation of the Wolf-Rayet and OB pair. If it is found to be at the same distance as the bright spectroscopic pair, it would likely be an F-type main sequence star in an orbit with a period around 100,000 years and the lowest-luminosity known companion of any WR star at Шаблон:Solar luminosity.[16]

References

Шаблон:Reflist

Further reading

Шаблон:Div col

Шаблон:Div col end

Шаблон:Stars of Serpens

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  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 Forbes2000 не указан текст
  4. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Fleming1892 не указан текст
  5. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Hiltner1945 не указан текст
  6. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Gaposchkin1949 не указан текст
  7. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Hjellming_Hiltner_1963 не указан текст
  8. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Stępień1970 не указан текст
  9. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Kuhi_Schweizer_1970 не указан текст
  10. ↑ 10,0 10,1 10,2 Ошибка цитирования Неверный тег <ref>; для сносок Hill_et_al_2018 не указан текст
  11. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Gonzalez_Rosado_1984 не указан текст
  12. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Lipunova1985 не указан текст
  13. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Antokhin_et_al_2000 не указан текст
  14. ↑ Ошибка цитирования Неверный тег <ref>; для сносок sen2020 не указан текст
  15. ↑ Ошибка цитирования Неверный тег <ref>; для сносок vanbeveren2018 не указан текст
  16. ↑ Ошибка цитирования Неверный тег <ref>; для сносок shara2022 не указан текст
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