论文标题
区分最大中子恒星质量的中子星和黑洞的中子星和黑洞
Discriminating between Neutron Stars and Black Holes with Imperfect Knowledge of the Maximum Neutron Star Mass
论文作者
论文摘要
尽管具有特殊低质量紧凑型二进制聚结的引力波信号，例如GW170817，可能会带有与二进制黑洞系统区分开的物质特征，但当前先进的Ligo和Vile Go观察者发现的每八个事件中，只有一个可能具有足够的信号效果，即使这些事件也可能具有足够的信号效果，即使这些事件也很大。尽管如此，系统的组件质量通常会受到限制。为合并紧凑物体的总速率密度构建明确的混合模型，我们根据后部的几率从不同的亚种群中得出其组分质量，以对重力波源进行分类。考虑到最大中子星质量的当前不确定性，并为总速率密度采用不同的合理模型，我们研究了Ligo-Virgo协作的第三次观察跑步GW190425和GW190814的两个最新事件。对于中子星和黑洞质量分布之间没有重叠的人口模型，我们通常会发现GW190425是二进制中子星合并，而不是中子星 - 布莱克孔合并。另一方面，我们发现GW190814涉及一个缓慢旋转的中子星，无论我们假设的人口模型如何，GW190814都有一个$ \ lyssim 6 \％$的机会。
Although gravitational-wave signals from exceptional low-mass compact binary coalescences, like GW170817, may carry matter signatures that differentiate the source from a binary black hole system, only one out of every eight events detected by the current Advanced LIGO and Virgo observatories are likely to have signal-to-noise ratios large enough to measure matter effects, even if they are present. Nonetheless, the systems' component masses will generally be constrained precisely. Constructing an explicit mixture model for the total rate density of merging compact objects, we develop a hierarchical Bayesian analysis to classify gravitational-wave sources according to the posterior odds that their component masses are drawn from different subpopulations. Accounting for current uncertainty in the maximum neutron star mass, and adopting different reasonable models for the total rate density, we examine two recent events from the LIGO-Virgo Collaboration's third observing run, GW190425 and GW190814. For population models with no overlap between the neutron star and black hole mass distributions, we typically find that there is a $\gtrsim 70\%$ chance that GW190425 was a binary neutron star merger rather than a neutron-star--black-hole merger. On the other hand, we find that there is a $\lesssim 6\%$ chance that GW190814 involved a slowly spinning neutron star, regardless of our assumed population model.
