Modeling the postmerger gravitational wave signal and extracting binary properties from future binary neutron star detections
Modeling the postmerger gravitational wave signal and extracting binary properties from future binary neutron star detections
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DOI：
10.1103/physrevd.100.044047
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发表时间：
2019-07
影响因子：
5
通讯作者：
K. W. Tsang;T. Dietrich;C. Broeck
中科院分区：
文献类型：
--
作者：
K. W. Tsang;T. Dietrich;C. Broeck
引力波天文学已经确立了它在测量支配冷核子物质的状态方程方面的作用。到目前为止，以及在不久的将来，中子星双星引力波的测量很可能仅限于激发波。然而，未来的升级和下一代引力波探测器将使我们能够探测到两颗恒星合并后发出的引力波信号，当密度达到单中子星的密度时。因此，合并后的引力波信号使研究处于极端极限的超核物质成为可能。为了支持这一研究路线，我们提出了并购后演化的二元属性和特征特征之间的新的和更新的现象学关系。最值得注意的是，我们得到了质量加权潮汐变形性和最大中子星质量与合并后光谱的主要发射频率之间的更新关系。通过使用简化的洛伦兹模型函数进行与构型无关的贝叶斯分析，我们发现，对于Advanced LIGO和Advanced Virgo的设计灵敏度，在信噪比为8及以上的情况下，可以在约100 Hz的1-sigma不确定度内提取合并后剩余的主发射频率。在某些情况下，即使合并后的信噪比为4也足以确定主发射频率。这将使我们能够测量合并后的双星和状态方程的性质，执行双星中子星合并的不同部分之间的一致性检查，并将我们对中子星合并的物理解释付诸实践。
Gravitational wave astronomy has established its role in measuring the equation of state governing cold supranuclear matter. To date and in the near future, gravitational wave measurements from neutron star binaries arc likely to be restricted to the inspiral. However, future upgrades and the next generation of gravitational wave detectors will enable us to detect the gravitational wave signatures emitted after the merger of two stars, at times when densities beyond those in single neutron stars are reached. Therefore, the postmerger gravitational wave signal enables studies of supranuclear matter at its extreme limit. To support this line of research, we present new and updated phenomenological relations between the binary properties and characteristic features of the postmerger evolution. Most notably, we derive an updated relation connecting the mass-weighted tidal deformability and the maximum neutron star mass to the dominant emission frequency of the postmerger spectrum. With the help of a configuration-independent Bayesian analysis using simplified Lorentzian model functions, we find that the main emission frequency of the postmerger remnant, for signal-to-noise ratios of 8 and above, can be extracted within a 1-sigma uncertainty of about 100 Hz for Advanced LIGO and Advanced Virgo's design sensitivities. In some cases, even a postmerger signal-to-noise ratio of 4 can be sufficient to determine the main emission frequency. This will enable us to measure binary and equation-of-state properties from the postmerger, to perform a consistency check between different parts of the binary neutron star coalescence, and to put our physical interpretation of neutron star mergers to the test.