On the possibility of disk-fed formation in supergiant high-mass X-ray binaries
On the possibility of disk-fed formation in supergiant high-mass X-ray binaries
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DOI：
10.1088/1674-4527/19/1/12
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发表时间：
2018-09
影响因子：
1.8
通讯作者：
Ali Taani;S. Karino;Liming Song;M. Al-Wardat;A. Khasawneh;M. Mardini
中科院分区：
文献类型：
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作者：
Ali Taani;S. Karino;Liming Song;M. Al-Wardat;A. Khasawneh;M. Mardini
我们利用探测到的回旋线来考虑中子星星磁场的存在。我们收集了九个来源的高质量X射线双星与超巨星的同伴作为我们的模型的测试案例的数据，以证明他们的分布和演化。研究了不同质量损失率下的风速、自旋周期和磁场强度。在我们的模型中，质量损失率和风速之间的相关性被发现，并可以在进一步的观测进行检验。我们检查风吸积允许的参数空间，避免旋转磁场的障碍，与强大的数据中子星的磁场。我们的模型表明，大多数源（九个系统中的六个）可以由风速相对较慢的风馈送，这一结果与以前的预测一致。在一些来源中，我们的模型不能适合标准的风吸积场景。在这些特殊的情况下，其他方案（磁盘形成，部分罗氏瓣溢出）应予以考虑。这将提供有关各种类型双星演化轨迹的信息，因此在风馈X射线双星系统中表现出明显的二分法行为。
We consider the existence of a neutron star magnetic field by the detected cyclotron lines. We collected data on nine sources of high-mass X-ray binaries with supergiant companions as a test case for our model, to demonstrate their distribution and evolution. The wind velocity, spin period and magnetic field strength are studied under different mass loss rates. In our model, correlations between mass-loss rate and wind velocity are found and can be tested in further observations. We examine the parameter space where wind accretion is allowed, avoiding the barrier of rotating magnetic fields, with robust data on the magnetic field of neutron stars. Our model shows that most sources (six of nine systems) can be fed by the wind with relatively slow velocity, and this result is consistent with previous predictions. In a few sources, our model cannot fit the standard wind accretion scenario. In these peculiar cases, other scenarios (disk formation, partial Roche lobe overflow) should be considered. This would provide information about the evolutionary tracks of various types of binaries, and thus exhibit a clear dichotomy behavior in wind-fed X-ray binary systems.