A global study of type B quasi-periodic oscillation in black hole X-ray binaries
A global study of type B quasi-periodic oscillation in black hole X-ray binaries
复制标题
黑洞X射线双星B型准周期振荡的全球研究
DOI：
10.1093/mnras/stw3146
复制
发表时间：
2017
影响因子：
4.8
通讯作者：
Gao H. Q. et al.
中科院分区：
文献类型：
--
作者：
Gao H. Q. et al.
我们对黑洞X射线双星爆发中的B类准周期振荡（QPO）的时间和光谱性质进行了全面的研究。该样本是基于Rossi X射线定时探测器（RXTE）的观测，通过搜索RXTE时代的文献中所有已识别的B型QPO来构建的。为了扩大样本，我们还研究了一些已报道但尚未完全确定的B型QPO。关于时滞和硬/软通量比，我们发现具有B类QPO的源表现为两个子群。在一个子组中，B型QPO显示出硬时间滞后，该硬时间滞后首先减小，然后随着能谱的软化而沿着反转成软时间滞后。在另一个亚组中，B型QPO只分布在一个小的区域，具有硬时滞和相对软的硬度。这些发现可以理解为不同来源的热内部流动的均匀性的多样性。我们证实了在不同的源中，B型QPO频率和硬分量亮度之间的正相关关系的普遍性。我们解释的结果，考虑到B型QPO光子产生的内部吸积流周围的中心黑洞，在当地爱丁顿限制。利用这个关系，我们得到了H1743 −322黑洞的质量估计为9.3-27.1 M_∞。
We performed a global study on the timing and spectral properties of type-B quasi-periodic oscillations (QPOs) in the outbursts of black hole X-ray binaries. The sample is built based on the observations of Rossi X-ray Timing Explorer (RXTE), via searching in the literature in RXTE era for all the identified type-B QPOs. To enlarge the sample, we also investigated some type-B QPOs that are reported but not yet fully identified. Regarding to the time lag and hard/soft flux ratio, we found that the sources with type-B QPOs behave in two subgroups. In one subgroup, type-B QPO shows a hard time lag that first decreases and then reverse into a soft time lag along with softening of the energy spectrum. In the other subgroup, type-B QPOs distribute only in a small region with hard time lag and relatively soft hardness. These findings may be understood with a diversity of the homogeneity showing up for the hot inner flow of different sources. We confirm the universality of a positive relation between the type-B QPO frequency and the hard component luminosity in different sources. We explain the results by considering that the type-B QPO photons are produced in the inner accretion flow around the central black hole, under a local Eddington limit. Using this relationship, we derived a mass estimation of 9.3–27.1 M_⊙ for the black hole in H 1743−322.