Detecting Black Hole Binaries by Gaia
Detecting Black Hole Binaries by Gaia
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DOI：
10.3847/1538-4357/aac5ec
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发表时间：
2017-10
期刊：
影响因子：
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通讯作者：
M. Yamaguchi;N. Kawanaka;T. Bulik;T. Piran
中科院分区：
文献类型：
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作者：
M. Yamaguchi;N. Kawanaka;T. Bulik;T. Piran
我们研究了盖亚卫星通过探测伴星的轨道运动来识别黑洞双星系统的前景。考虑到初始质量函数，质量传递，共同的包络相，星际吸收，和系统的可识别性，我们估计的BH双星的数量，可以检测到的盖亚和他们的分布相对于BH质量。考虑几种不同参数的模型，我们发现盖亚在其2005年的运行中可以探测到2000 -1000个BH双星。BH质量分布函数的形状强烈地受零龄主序星质量-BH质量关系的影响。我们表明，一旦这个分布是建立观测，我们将能够约束目前未知的ZAMS质量BH质量关系。
We study the prospects of the Gaia satellite to identify black hole (BH) binary systems by detecting the orbital motion of the companion stars. Taking into account the initial mass function, mass transfer, common envelope phase, interstellar absorption, and identifiability of the systems, we estimate the number of BH binaries that can be detected by Gaia and their distributions with respect to the BH mass. Considering several models with different parameters, we find that ∼200–1000 BH binaries could be detected by Gaia during its ∼5 years operation. The shape of the BH mass distribution function is affected strongly by the zero-age main sequence (ZAMS) stellar mass–BH mass relation. We show that once this distribution is established observationally, we will be able to constrain the currently unknown ZAMS mass–BH mass relation.