Kicking gravitational wave detectors with recoiling black holes
Kicking gravitational wave detectors with recoiling black holes
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DOI：
10.1103/physrevd.100.104039
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发表时间：
2019-08
影响因子：
5
通讯作者：
C. Lousto;J. Healy
中科院分区：
文献类型：
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作者：
C. Lousto;J. Healy
双黑洞发出具有净线性动量的引力辐射，导致最终残余黑洞的后退，可达 $\sim5,000$ km/s。完整的数值相对论模拟是准确计算这些反冲的唯一工具，因为它们主要是在黑洞视界即将合并时产生的，并且强烈依赖于当时的自旋方向。我们提出了悬挂踢配置系列中 BBH 的八个新数值模拟，可产生最大后坐力。黑洞质量相等且接近最大旋转 ($|\vec{S}_{1,2}|/m_{1,2}^2=0.97$)。根据合并时的相位，该族导致 $\sim\pm4,700$ km/s 以及沿双星系统轨道角动量的反冲的所有中间值。我们引入了一种新的不变方法，通过用作参考相位角的波形峰值幅度来评估反冲对合并相位的依赖性，并将其与以前的定义进行比较。我们还计算这些挂断踢波形之间的不匹配，以通过引力波探测器（例如先进的 LIGO）推断它们的可观测微分性，找到当前可达到的信噪比，从而允许识别具有其他基本相同的二进制参数的高反冲黑洞。
Binary black holes emit gravitational radiation with net linear momentum leading to a retreat of the final remnant black hole that can reach up to $\sim5,000$ km/s. Full numerical relativity simulations are the only tool to accurately compute these recoils since they are largely produced when the black hole horizons are about to merge and they are strongly dependent on their spin orientations at that moment. We present eight new numerical simulations of BBH in the hangup-kick configuration family, leading to the maximum recoil. Black holes are equal mass and near maximally spinning ($|\vec{S}_{1,2}|/m_{1,2}^2=0.97$). Depending on their phase at merger, this family leads to $\sim\pm4,700$ km/s and all intermediate values of the recoil along the orbital angular momentum of the binary system. We introduce a new invariant method to evaluate the recoil dependence on the merger phase via the waveform peak amplitude used as a reference phase angle and compare it with previous definitions. We also compute the mismatch between these hangup-kick waveforms to infer their observable differentiability by gravitational wave detectors, such as advanced LIGO, finding currently reachable signal-to-noise ratios, hence allowing for the identification of highly recoiling black holes having otherwise essentially the same binary parameters.