Aligned spin neutron star-black hole mergers: A gravitational waveform amplitude model
Aligned spin neutron star-black hole mergers: A gravitational waveform amplitude model
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对齐的自旋中子星-黑洞合并：引力波形振幅模型
DOI：
10.1103/physrevd.92.084050
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发表时间：
2015
影响因子：
5
通讯作者：
Masaru Shibata
中科院分区：
文献类型：
--
作者：
Francesco Pannarale;Emanuele Berti;Koutarou Kyutoku;Benjamin D. Lackey;Masaru Shibata
黑洞和中子星合并时发出的引力辐射与中子星不受潮汐破坏时两个黑洞合并时的辐射非常相似。当发生潮汐扰动时，重力波形可以大致分为两组，这取决于被扰动物质的空间范围。扩展了我们一些人之前的工作，在这里，我们提出了一个频率域中引力波形幅度的唯象模型，包括合并的三种可能结果：没有潮汐干扰，以及“温和”和“强烈”的潮汐干扰。该模型被校准到134个双星的广义相对论数值模拟，其中黑洞自转与轨道角动量对齐或反对齐。所有的模拟都是使用SACRA码和分段多变中子星状态方程进行的。本模型可以用来确定黑洞二进制波形何时足以探测引力波，从未来的引力波观测中提取关于状态方程的信息，获得更准确的黑洞-中子星合并事件率估计，并确定这些系统作为伽马射线暴和宏新星/千新星的中心引擎的条件。
The gravitational radiation emitted during the merger of a black hole with a neutron star is rather similar to the radiation from the merger of two black holes when the neutron star is not tidally disrupted. When tidal disruption occurs, gravitational waveforms can be broadly classified in two groups, depending on the spatial extent of the disrupted material. Extending previous work by some of us, here we present a phenomenological model for the gravitational waveform amplitude in the frequency domain encompassing the three possible outcomes of the merger: no tidal disruption, and “mild” and “strong” tidal disruption. The model is calibrated to 134 general-relativistic numerical simulations of binaries where the black hole spin is either aligned or antialigned with the orbital angular momentum. All simulations were produced using theSACRAcode and piecewise polytropic neutron star equations of state. The present model can be used to determine when black-hole binary waveforms are sufficient for gravitational-wave detection, to extract information on the equation of state from future gravitational-wave observations, to obtain more accurate estimates of black hole-neutron star merger event rates, and to determine the conditions under which these systems are plausible candidates as central engines of gamma-ray bursts and macronovae/kilonovae.