The formation of black hole low-mass X-ray binaries: through case B or case C mass transfer?
The formation of black hole low-mass X-ray binaries: through case B or case C mass transfer?
复制标题
黑洞低质量X射线双星的形成：通过案例B还是案例C传质？
DOI：
10.1051/0004-6361:20010949
复制
发表时间：
2001
影响因子：
6.5
通讯作者：
E. Heuvel
中科院分区：
文献类型：
--
作者：
G. Nelemans;E. Heuvel
包含相当大质量（$M \ga 7 M_{\odot}$）黑洞的低质量X射线双星的形成是有问题的，因为在最近的恒星演化计算中，这些黑洞的直接祖先（沃尔夫-拉叶星）通过恒星风损失了如此多的质量，以至于它们的最终质量远低于观测到的黑洞质量。我们讨论了最近提出的解决方案，即这些双星是通过案例 C 传质（即核心氦燃烧完成后的传质）形成的，避免了较长的沃尔夫-拉叶相，从而避免了显着的质量损失。我们表明，只有一些当前可用的大质量恒星演化模型允许这种形成通道。我们还研究了观测结果表明的向下修正的沃尔夫-拉叶质量损失率的影响，并得出结论，在这种情况下，沃尔夫-拉叶恒星以比之前发现的显着更高的质量结束生命，并且可能能够形成黑洞。
The formation of low-mass X-ray binaries containing a rather massive ($M \ga 7 M_{\odot}$) black hole is problematic because in most recent stellar evolutionary calculations the immediate progenitors of these black holes (Wolf-Rayet stars) lose so much mass via their stellar wind that their final masses are well below the observed black hole masses. We discuss the recently proposed solution that these binaries are formed through case C mass transfer (i.e. mass transfer after core helium burning is completed), avoiding a long Wolf-Rayet phase and thus significant mass loss. We show that only some of the currently available models for the evolution of massive stars allow this formation channel. We also investigate the effect of the downward revised Wolf-Rayet mass-loss rate as is suggested by observations, and conclude that in that case Wolf-Rayet stars end their lives with significantly higher masses than previously found and may be able to form a black holes.