论文标题
比较灵感，准圆形和非启动黑洞二进制文件的二阶引力自我和有效的一个体波形II：大型质量案例
Comparing second-order gravitational self-force and effective one body waveforms from inspiralling, quasi-circular and nonspinning black hole binaries II: the large-mass-ratio case
论文作者
论文摘要
我们将最近计算出的波形从二阶引力自我（GSF）理论与由新的，有效的，有效的一个身体（EOB）波形模型产生的波形与（自旋平衡，偏心）具有较大质量比的黑洞二进制组所产生的波形。我们专注于准圆形，非插入，配置，并执行详细的GSF/EOB波形相结合比较，无论是在时域还是通过量规不变的尺寸无量纲函数$q_Ω\equivΩ^2/\dotΩ，其中$ω$，其中$ω$是prestitation Wave频率。在EOB辐射反应中包含高PN测试量术语（值得注意的是，高达22pn）对于达到1 〜1降低至1次的EOB/GSF相位一致性至关重要，直到质量比的质量比最高为500。对于较大的质量比率，较大的质量比，最高$ 5 \ \ \ \ \ \ \ \ \ \ $ 5 \ \ \ $ 5 \ times 10^4 $，并且需要更重要的是，它的贡献是更重要的，并且需要更重要的是重要的。我们的结果表明，我们的GSF信息EOB波形模型是描述由中间或极端质量比的波形的有前途的工具
We compare recently computed waveforms from second-order gravitational self-force (GSF) theory to those generated by a new, GSF-informed, effective one body (EOB) waveform model for (spin-aligned, eccentric) inspiralling black hole binaries with large mass ratios. We focus on quasi-circular, nonspinning, configurations and perform detailed GSF/EOB waveform phasing comparisons, either in the time domain or via the gauge-invariant dimensionless function $Q_ω\equiv ω^2/\dotω$, where $ω$ is the gravitational wave frequency. The inclusion of high-PN test-mass terms within the EOB radiation reaction (notably, up to 22PN) is crucial to achieve an EOB/GSF phasing agreement below 1~rad up to the end of the inspiral for mass ratios up to 500. For larger mass ratios, up to $5\times 10^4$, the contribution of horizon absorption becomes more and more important and needs to be accurately modeled. Our results indicate that our GSF-informed EOB waveform model is a promising tool to describe waveforms generated by either intermediate or extreme mass ratio inspirals for future gravitational wave detectors
