Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: Comparable mass, nonspinning case
Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: Comparable mass, nonspinning case
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DOI：
10.1103/physrevd.103.064022
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发表时间：
2021-01
影响因子：
5
通讯作者：
Tousif Islam;V. Varma;Jackie Lodman;Scott E. Field;G. Khanna;M. Scheel;H. Pfeiffer;D. Gerosa;Lawrence E. Kidder
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作者：
Tousif Islam;V. Varma;Jackie Lodman;Scott E. Field;G. Khanna;M. Scheel;H. Pfeiffer;D. Gerosa;Lawrence E. Kidder
我们开发了新的策略来建立偏心双黑洞系统的数值相对论代理模型，预计将在当前和未来的引力波探测器中发挥越来越重要的作用。我们引入了一个新的替代波形模型，\texttt{NRSur 2dq 1 Ecc}，使用47 nonspinning，等质量波形的偏心率高达0.2 $时，在合并前的参考时间为55亿美元。这是第一个直接在偏心数值相对论模拟上训练的波形模型，并且不需要在合并之前进行二进制循环。该模型包括$（2，2）$，$（3，2）$和$（4，4）$自旋加权球谐模。我们还建立了一个最终的黑洞模型，\texttt{NRSur 2dq 1 EccRemnant}，它模拟了残余黑洞的质量和自旋。结果表明，我们的波形模型可以准确地预测数值相对论波形，误差为$\approximat 10^{-3}$，而残余模型可以恢复最终质量和无量纲自旋，绝对误差分别小于$\approximat 5 \times 10^{-4}M$和$\approximat 2\times 10 ^{-3}$.我们表明，波形模型也可以恢复微妙的效果，如模式混合的振铃信号，没有任何特殊的特设建模步骤。最后，我们表明，尽管只在等质量的二进制文件上训练，\texttt{NRSur 2dq 1 Ecc}可以合理地扩展到质量比$q\approx3$与不匹配$\simeq 10^{-2}$的偏心率小于$\sim 0.05$作为测量的参考时间$2000 M $合并前。这里开发的方法应证明是有用的，在未来的偏心代理模型的参数空间的更大的区域的建设。
We develop new strategies to build numerical relativity surrogate models for eccentric binary black hole systems, which are expected to play an increasingly important role in current and future gravitational-wave detectors. We introduce a new surrogate waveform model, \texttt{NRSur2dq1Ecc}, using 47 nonspinning, equal-mass waveforms with eccentricities up to $0.2$ when measured at a reference time of $5500M$ before merger. This is the first waveform model that is directly trained on eccentric numerical relativity simulations and does not require that the binary circularizes before merger. The model includes the $(2,2)$, $(3,2)$, and $(4,4)$ spin-weighted spherical harmonic modes. We also build a final black hole model, \texttt{NRSur2dq1EccRemnant}, which models the mass, and spin of the remnant black hole. We show that our waveform model can accurately predict numerical relativity waveforms with mismatches $\approx 10^{-3}$, while the remnant model can recover the final mass and dimensionless spin with absolute errors smaller than $\approx 5 \times 10^{-4}M$ and $\approx 2 \times10^{-3}$ respectively. We demonstrate that the waveform model can also recover subtle effects like mode-mixing in the ringdown signal without any special ad-hoc modeling steps. Finally, we show that despite being trained only on equal-mass binaries, \texttt{NRSur2dq1Ecc} can be reasonably extended up to mass ratio $q\approx3$ with mismatches $\simeq 10^{-2}$ for eccentricities smaller than $\sim 0.05$ as measured at a reference time of $2000M$ before merger. The methods developed here should prove useful in the building of future eccentric surrogate models over larger regions of the parameter space.