在引力波观测中识别黑洞：在质量间隙双星中区分冒名顶替者的挑战
Recognizing black holes in gravitational-wave observations: Challenges in telling apart impostors in mass-gap binaries
摘要：
本文研究了如何通过对地基引力波探测器中致密双星的内旋信号中潮汐变形性（TD）和潮汐加热（TH）的仔细监测，来检验其组成部分是否为黑洞。前者的性质（TD）是有限的中子星，但黑洞（在广义相对论中）消失，而后者是有限的黑洞和中子星可以忽略不计，并影响GW阶段的演化的双星以一个明显不同的方式。我们引入波形参数来表征潮汐加热的强度，并且当没有地平线时为零。我们开发了贝叶斯方法，使用TD和TH来区分二元中是否存在层位。这是及时的，因为有几种说法认为，这些恒星质量的物体，特别是质量比中子星重的物体，可能没有视界，但可能是黑洞模仿者或奇异的紧凑物体（ECO）。在天体物理学上，拥有测试质量间隙双星中是否存在视界的工具也很重要，从而有助于探测最重的中子星或最轻的黑洞。在双星波形模型中对潮汐加热进行适当的解释，对于在对包含它们的双星进行GW观测时对中子星状态方程特性进行无偏测量，甚至探测ECO的存在，也是至关重要的。我们表明，纯粹的GW波形的基础上，它将是不可能辨别二进制地平线的质量差距在先进的LIGO，处女座和KAGRA探测器，除非二进制是在几十Mpc。然而，第三代地基探测器将能够对几百兆秒差距的双星进行探测。
英文摘要：
We study how by careful monitoring of the presence or absence of tidal deformability (TD) and tidal-heating (TH) in the inspiral signal of compact object binaries in ground-based gravitational wave (GW) detectors, one can test if its components are black holes or not. The former property (TD) is finite for neutron stars but vanishes for black holes (in general relativity), whereas the latter is finite for black holes and negligible for neutron stars, and affects the GW phase evolution of binaries in a distinctly different way. We introduce waveform parameters that characterize the strength of tidal-heating, and are zero when there is no horizon. We develop Bayesian methods that use TD and TH for distinguishing the presence or absence of horizons in a binary. This is timely owing to several claims that these stellar-mass objects, especially, with masses heavier than those of neutron stars, may not have a horizon but may be black hole mimickers or exotic compact objects (ECOs). It is also astrophysically important to have the tools to test the presence or absence of horizons in mass-gap binaries and, thereby, help detect the heaviest neutron star or the lightest black hole. A proper accounting of tidal-heating in binary waveform models will also be critical for an unbiased measurement of characteristics of the equation of state of neutron stars in GW observations of binaries containing them -- or even to probe the existence of ECOs. We show that purely based on GW waveforms it will not be possible to discern binary horizons in the mass gap in Advanced LIGO, Virgo and KAGRA detectors unless the binary is within a few tens of Mpc. However, third generation ground-based detectors will be able to do so for binaries a few hundred Mpc away.
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