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Formation of the black-hole binary M33 X-7 through mass exchange in a tight massive system
Valsecchi, Francesca1,2; Glebbeek, Evert3; Farr, Will M.1,2; Fragos, Tassos1,2,6; Willems, Bart1,2; Orosz, Jerome A.4; Liu, Jifeng5,6; Kalogera, Vassiliki1,2
2010-11-04
发表期刊NATURE
卷号468期号:7320页码:77-79
摘要The X-ray source M33 X-7 in the nearby galaxy Messier 33 is among the most massive X-ray binary stellar systems known, hosting a rapidly spinning, 15.65M(circle dot) black hole orbiting an underluminous, 70M(circle dot) main-sequence companion in a slightly eccentric 3.45-day orbit(1,2) (M(circle dot), solar mass). Although post-main-sequence mass transfer explains the masses and tight orbit(3), it leaves unexplained the observed X-ray luminosity, the star's underluminosity, the black hole's spin and the orbital eccentricity. A common envelope phase(1), or rotational mixing(4), could explain the orbit, but the former would lead to a merger and the latter to an overluminous companion. A merger would also ensue if mass transfer to the black hole were invoked for its spin-up(5). Here we report simulations of evolutionary tracks which reveal that if M33 X-7 started as a primary body of 85M(circle dot)-99M(circle dot) and a secondary body of 28M(circle dot)-32M(circle dot), in a 2.8-3.1-d orbit, its observed properties can be consistently explained. In this model, the main-sequence primary transfers part of its envelope to the secondary and loses the rest in a wind; it ends its life as a 16M(circle dot) helium star with an iron-nickel core that collapses to a black hole (with or without an accompanying supernova). The release of binding energy, and possibly collapse asymmetries, 'kick' the nascent black hole into an eccentric orbit. Wind accretion explains the X-ray luminosity, and the black-hole spin can be natal.
DOI10.1038/nature09463
收录类别SCI
语种英语
WOS记录号WOS:000283786900038
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文献类型期刊论文
条目标识符http://ir.bao.ac.cn/handle/114a11/7700
专题光学天文研究部
作者单位1.Northwestern Univ, CIERA, Evanston, IL 60208 USA
2.Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA
3.McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada
4.San Diego State Univ, Dept Astron, San Diego, CA 92182 USA
5.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
6.Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
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Valsecchi, Francesca,Glebbeek, Evert,Farr, Will M.,et al. Formation of the black-hole binary M33 X-7 through mass exchange in a tight massive system[J]. NATURE,2010,468(7320):77-79.
APA Valsecchi, Francesca.,Glebbeek, Evert.,Farr, Will M..,Fragos, Tassos.,Willems, Bart.,...&Kalogera, Vassiliki.(2010).Formation of the black-hole binary M33 X-7 through mass exchange in a tight massive system.NATURE,468(7320),77-79.
MLA Valsecchi, Francesca,et al."Formation of the black-hole binary M33 X-7 through mass exchange in a tight massive system".NATURE 468.7320(2010):77-79.
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