Английская Википедия:HD 136138

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Версия от 03:01, 18 марта 2024; EducationBot (обсуждение | вклад) (Новая страница: «{{Английская Википедия/Панель перехода}} {{Short description|Star in the constellation Serpens}} {{Starbox begin}} {{Starbox observe | epoch = J2000.0 | constell = Serpens | ra = {{RA|15|18|24.507}}<ref name=GaiaEDR3/> | dec = {{DEC|+20|34|21.95}}<ref name=GaiaEDR3/> | appmag_v = 5.68<ref name=Anderson_Francis_2012/> + 15.3<ref name=Holberg_et_al_2013/> }} {{Starbox character | type...»)
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HD 136138, or HR 5692, is a binary star system in the Serpens Caput segment of the Serpens constellation. It has a golden hue like the Sun and is dimly visible to the naked eye with an apparent visual magnitude of 5.68;[1] the light contribution from the companion is effectively negligible.[2] This system is located at a distance of approximately 420 light years from the Sun based on parallax.[3] It is drifting closer with a radial velocity of −7.7 km/s[1] and has a proper motion of Шаблон:Val·yr−1.[2]

The radial velocity variation of this star was reported by J. R. de Medeiros and M. Mayor in 1999,[4] and it was confirmed as a binary by A. Frankowski and colleagues in 2007 using proper motion measurements.[5] It is an unresolved, single-lined spectroscopic binary system with an orbital period of Шаблон:Convert and an eccentricity (ovalness) of 0.335. Proper motion measurements allow an estimate of the orbital inclination angle as ~43°.[6] Their semimajor axis is around Шаблон:Val, or double the distance from the Earth to the Sun.[2]

The stellar classification of the primary component is G8IIIa,[7] indicating this is a evolved G-type giant star that has exhausted the supply of hydrogen at its core. It is a red clump giant that is generating energy through core helium fusion. There is some ambiguous evidence for this being a mild barium star[6] of class Ba0.3,[2] with the spectra showing marginal overabundances of s-process elements.[2] A low level of X-ray emission has been detected, which appears to be coming from the star's corona.[8]

The high level of ultraviolet flux coming from this system strongly suggests the companion is a compact white dwarf. Mass estimates put it in the range of 0.6 to 0.8 times the mass of the Sun, and the temperature is around 30,400 K.[6] It is possible that the earlier evolution of this component contaminated its partner with s-process elements, although the resulting interaction should have circularized the orbit to some degree.[4] The dwarf has a visual magnitude of 15.3 and a hydrogen-dominated atmospheric class of DA1.7.[5]

References

Шаблон:Reflist

Шаблон:Stars of Serpens

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Разное

  1. ↑ 1,0 1,1 Ошибка цитирования Неверный тег <ref>; для сносок Anderson_Francis_2012 не указан текст
  2. ↑ 2,0 2,1 2,2 2,3 2,4 Ошибка цитирования Неверный тег <ref>; для сносок Merle2016 не указан текст
  3. ↑ Ошибка цитирования Неверный тег <ref>; для сносок GaiaEDR3 не указан текст
  4. ↑ 4,0 4,1 Ошибка цитирования Неверный тег <ref>; для сносок Griffin2009 не указан текст
  5. ↑ 5,0 5,1 Ошибка цитирования Неверный тег <ref>; для сносок Holberg_et_al_2013 не указан текст
  6. ↑ 6,0 6,1 6,2 Ошибка цитирования Неверный тег <ref>; для сносок Stefanik_et_al_2011 не указан текст
  7. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Keenan_McNeil_1989 не указан текст
  8. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Jorissen_et_al_1996 не указан текст
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