苹果和橘子：X射线双星和引力波源中黑洞的比较
Apples and Oranges: Comparing black holes in X-ray binaries and gravitational-wave sources
摘要：
在引力波（GW）双星黑洞（BBH）事件中观测到的分量黑洞（BH）比在黑洞X射线双星（BH-XRB）中观测到的分量黑洞（BH）质量更大，旋转速度更慢。没有模拟他们的进化历史，我们调查这些明显的紧张局势在BH人口是否可以解释GW观测选择效应。我们发现，这确实是在BBHs和观察到的高质量X射线双星（HMXB）的BH质量之间的差异的情况下，当我们考虑到统计不确定性，从小样本量的只有三个HMXB。另一方面，观测到的低质量X射线双星（LMXB）中的黑洞明显轻于天体物理学中的黑洞，但这可能只是由于双星系统中组件质量之间的相关性。考虑到它们的轻恒星同伴，我们预计LMXB中的轻BH。然而，在HMXB和LMXB中观察到的自旋与在$>99.9\%$水平上推断的BBH自旋分布存在张力。我们讨论了在观测到的BH-XRB中显着较大的自旋背后可能的情况。一种可能性是BBH的一个小的亚群（保守地说是$<30\%$）具有快速旋转的初级组分，表明它们可能遵循与观察到的HMXB相似的进化途径。在LMXBs中，有人认为黑洞可以通过吸积来加速旋转。如果LMXB的出生自旋遵循BBH自旋分布，我们发现LMXB的平均无量纲自旋为$0.47^{+0.10}_{-0.11}$，但如果它们的出生自旋遵循观测到的HMXB自旋，则平均自旋上升为$<0.03$。
英文摘要：
The component black holes (BHs) observed in gravitational-wave (GW) binary black hole (BBH) events tend to be more massive and slower spinning than those observed in black hole X-ray binaries (BH-XRBs). Without modeling their evolutionary histories, we investigate whether these apparent tensions in the BH populations can be explained by GW observational selection effects alone. We find that this is indeed the case for the discrepancy between BH masses in BBHs and the observed high-mass X-ray binaries (HMXBs), when we account for statistical uncertainty from the small sample size of just three HMXBs. On the other hand, the BHs in observed low-mass X-ray binaries (LMXBs) are significantly lighter than the astrophysical BBH population, but this may just be due to a correlation between component masses in a binary system. Given their light stellar companions, we expect light BHs in LMXBs. The observed spins in HMXBs and LMXBs, however, are in tension with the inferred BBH spin distribution at the $>99.9\%$ level. We discuss possible scenarios behind the significantly larger spins in observed BH-XRBs. One possibility is that a small subpopulation (conservatively $<30\%$) of BBHs have rapidly spinning primary components, indicating that they may have followed a similar evolutionary pathway to the observed HMXBs. In LMXBs, it has been suggested that BHs can spin up by accretion. If LMXB natal spins follow the BBH spin distribution, we find LMXBs must gain an average dimensionless spin of $0.47^{+0.10}_{-0.11}$, but if their natal spins follow the observed HMXB spins, the average spinup must be $<0.03$.
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