Английская Википедия:CX Draconis

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Шаблон:Short description 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

CX Draconis is an interacting binary star system in the northern constellation of Draco, abbreviated CX Dra. It has the designation HD 174237 in the Henry Draper Catalogue; CX Draconis is the variable star designation. This is a double-lined spectroscopic binary system with a near circular orbit.[1] The brightness of the system undergoes long-term irregular fluctuations,[2] ranging from an apparent visual magnitude of 5.68 down to 5.99.[3] Based on parallax measurements, it is located at a distance of approximately 1,150 light years from the Sun.[4]

In 1921, this target was found to have a varying radial velocity by J. S. Plaskett and associates.[5][6] It was shown to be a Be star by O. C. Mohler in 1940,[7] and in 1965 M. Lacoarret studied variations in the hydrogen alpha emission profiles from the target. This system was discovered to be a photometric variable by P. Merlin in 1975.[6] P. Koubský measured the radial velocity variations in 1976,[8] and in 1978 published orbital elements for this binary system with a period of 6.696 days.[9] He found that the variation in emission lines matched the time scale of the orbit, indicating that this is an interacting binary.[2]

Using observations from the Einstein Observatory, in 1984 this system was shown to be an X-ray source by E. F. Guinan and associates. This emission may be coming from the cooler secondary that is phase-locked with the primary and is magnetically active due to rapid rotation.[10] In 1992, J. Horn and associates determined that the secondary component is an evolved F-type giant star. Evidence suggests this star is overflowing its Roche lobe with gas streaming toward the primary.[2]

Models indicate that the main source of the H-alpha emission is located mid-way between the two stars, with other emission lines originating from an accretion disk orbiting the primary. The circumstellar environment is changing in cycles lasting hundreds of days.[1] Infrared emission to the northeast of the system suggests it may be undergoing systematic mass loss.[11]

References

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Further reading

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Шаблон:Stars of Draco

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  1. ↑ 1,0 1,1 Ошибка цитирования Неверный тег <ref>; для сносок Richards_et_al_2000 не указан текст
  2. ↑ 2,0 2,1 2,2 Ошибка цитирования Неверный тег <ref>; для сносок Horn_et_al_1992 не указан текст
  3. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Samus_et_al_2017 не указан текст
  4. ↑ Ошибка цитирования Неверный тег <ref>; для сносок GaiaEDR3 не указан текст
  5. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Plaskett_et_al_1921 не указан текст
  6. ↑ 6,0 6,1 Ошибка цитирования Неверный тег <ref>; для сносок Merlin_1975 не указан текст
  7. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Mohler_1940 не указан текст
  8. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Koubsky_1976 не указан текст
  9. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Koubsky_1978 не указан текст
  10. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Guinan_et_al_1984 не указан текст
  11. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Mayer_et_al_2016 не указан текст
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