Characterization of numerical relativity waveforms of eccentric binary black hole mergers
Characterization of numerical relativity waveforms of eccentric binary black hole mergers
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DOI：
10.1103/physrevd.100.044016
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发表时间：
2019-04
影响因子：
5
通讯作者：
Sarah Habib;E. Huerta
中科院分区：
文献类型：
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作者：
Sarah Habib;E. Huerta
我们介绍了一种方法来量化初始偏心率，引力波频率，和平均异常的数值相对论模拟，描述非旋转的黑洞在中等偏心轨道。我们证明，这种方法提供了一个强大的特性偏心二黑洞合并的质量比$q\leq10$和偏心率$e_0\leq0.2 $15个周期前合并。通过计算与准圆相对论波形的重叠量，对文献[1]中介绍的各种偏心数值相对论波形的圆化率进行了量化，发现它们在合并前的重叠量为50 M $，为中等偏心质量比的二元黑洞合并的圆化提供了证据.我们还量化的重要性，包括高阶波形模式的偏心二进制黑洞合并的表征。使用两种类型的数值波形，一种包括$（\ell，\，|M|）= \{（2，\，2），\，（2，\，1），\，（3，\，3），\，（3，\，2），\，（3，\，1），\，（4，\，4），\，（4，\，3），\，（4，\，2），\，（4，\，1）\}$和仅包括$\ell=| M| =2$模式，我们发现，这两类波形之间的重叠低至${\cal{O}}=0.89$为$q=10$偏心二元黑洞合并，强调需要包括高阶波形模式的描述这些引力波源。我们讨论了这些发现对未来源建模和引力波探测工作的影响。
We introduce a method to quantify the initial eccentricity, gravitational wave frequency, and mean anomaly of numerical relativity simulations that describe non-spinning black holes on moderately eccentric orbits. We demonstrate that this method provides a robust characterization of eccentric binary black hole mergers with mass-ratios $q\leq10$ and eccentricities $e_0\leq0.2$ fifteen cycles before merger. We quantify the circularization rate of a variety of eccentric numerical relativity waveforms introduced in [1] by computing overlaps with their quasi-circular counterparts, finding that $50M$ before merger they attain overlaps ${\cal{O}}\geq0.99$, furnishing evidence for the circularization of moderately eccentric binary black hole mergers with mass-ratios $q\leq10$. We also quantify the importance of including higher-order waveform modes for the characterization of eccentric binary black hole mergers. Using two types of numerical waveforms, one that includes $(\ell, \, |m|)= \{(2,\,2),\, (2,\,1),\, (3,\,3),\, (3,\,2), \, (3,\,1),\, (4,\,4),\, (4,\,3),\, (4,\,2),\,(4,\,1)\}$ and one that only includes the $\ell=|m|=2$ mode, we find that the overlap between these two classes of waveforms is as low as ${\cal{O}}=0.89$ for $q=10$ eccentric binary black hole mergers, underscoring the need to include higher-order waveform modes for the description of these gravitational wave sources. We discuss the implications of these findings for future source modeling and gravitational wave detection efforts.