Numerical relativity higher order gravitational waveforms of eccentric, spinning, nonprecessing binary black hole mergers
Numerical relativity higher order gravitational waveforms of eccentric, spinning, nonprecessing binary black hole mergers
复制标题
DOI：
10.1103/physrevd.107.064038
复制
发表时间：
2022-10
影响因子：
5
通讯作者：
A. Joshi;S. Rosofsky;R. Haas;E. Huerta
中科院分区：
文献类型：
--
作者：
A. Joshi;S. Rosofsky;R. Haas;E. Huerta
我们使用开源的、社区驱动的、数值相对论软件Einstein Toolkit来研究偏心的、旋转的、非旋进的双黑洞合并的物理学，其中质量比q=\{2，4，6\}$，单个无量纲自旋参数$\chi_{1 z}=\pm0.6$，$\chi_{2 z}=\pm0.3$，包括高阶引力波模式$\ell\leq4 $，除了存储器模式。假设恒星质量的二进制黑洞合并，可以检测到先进的LIGO探测器，我们发现，包括模式高达$\ell=4$增加了信号噪声之间的紧凑的二进制3.5\%$至35\%$，相比之下，信号，只包括$\ell=| M| =2$模式。我们使用两个波形模型，TEOBResumS和SEOBNRE，其中包括自旋和偏心率校正的波形动力学，量化的轨道偏心率的数值相对论目录规范不变的方式，通过拟合因子计算。我们的研究结果表明，包含高阶波模式有一个可测量的影响，在恢复中度和高度偏心黑洞合并，因此，它是必不可少的开发波形模型和信号处理工具，准确地描述这些天体物理源的物理。
We use the open source, community-driven, numerical relativity software, the Einstein Toolkit to study the physics of eccentric, spinning, nonprecessing binary black hole mergers with mass-ratios $q=\{2, 4, 6\}$, individual dimensionless spin parameters $\chi_{1z}=\pm0.6$, $\chi_{2z}=\pm0.3$, that include higher order gravitational wave modes $\ell\leq4$, except for memory modes. Assuming stellar mass binary black hole mergers that may be detectable by the advanced LIGO detectors, we find that including modes up to $\ell=4$ increases the signal-to-noise of compact binaries between $3.5\%$ to $35\%$, compared to signals that only include the $\ell=|m|=2$ mode. We use two waveform models, TEOBResumS and SEOBNRE, which incorporate spin and eccentricity corrections in the waveform dynamics, to quantify the orbital eccentricity of our numerical relativity catalog in a gauge-invariant manner through fitting factor calculations. Our findings indicate that the inclusion of higher order wave modes has a measurable effect in the recovery of moderately and highly eccentric black hole mergers, and thus it is essential to develop waveform models and signal processing tools that accurately describe the physics of these astrophysical sources.