arXiv 2601.033402026-01-14gr-qcastro-ph.HE

快速频域现象学建模：偏心对齐自旋二体黑洞

Fast frequency-domain phenomenological modeling of eccentric aligned-spin binary black holes

National Institute for Subatomic Physics (Nikhef)（荷兰亚原子物理国家研究所）

Antoni Ramos-Buades, Quentin Henry, Maria Haney

备注：: Updated acknowledgements

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AI总结：

IMRPhenomXE是一种快速频域现象学建模方法，用于偏心对齐自旋二体黑洞的波形建模，具有高精度和效率。

摘要：

我们提出了IMRPhenomXE频域现象学波形模型，用于椭圆轨道上非进动二黑洞的主导模式。IMRPhenomXE扩展了用于主导(ℓ,|m|)=(2,2)模式的准圆形IMRPhenomXAS波形模型，以适应偏心二体。在进动部分，采用准开普勒参数化在准开普勒参数化中，直到第三后牛顿阶的轨道平均运动方程，包括自旋效应，被演算，波形模式通过使用静止相位近似在偏心性展开表达式中计算到O(e^{12})。该模型假设在并合-环形阶段圆化，其中它采用底层准圆形IMRPhenomXAS基础线。我们证明IMRPhenomXE在准圆形极限下还原为准确的IMPhenomXAS模型。与186个公开的数值广义相对论波形从Simulating eXtreme Spacetimes目录中相比，初始偏心率最高达到约0.8，IMRPhenomXE在初始偏心率低于0.4的72%的模拟中提供了小于3%的不忠实度。对于较大的偏心率，不忠实度下降到大于10%，这是由于底层的小偏心率展开和额外的建模近似。在速度方面，IMRPhenomXE优于现有的所有进动-并合-环形偏心波形模型。我们通过将IMRPhenomXE注入零噪声和参数估计分析中，展示了其效率、稳健性和模块性，表明IMRPhenomXE是用于引力波天文学在快速增长的事件目录时代的即用型波形模型。

英文摘要：

We present the IMRPhenomXE frequency-domain phenomenological waveform model for the dominant mode of inspiral-merger-ringdown non-precessing binary black holes in elliptical orbits. IMRPhenomXE extends the quasi-circular IMRPhenomXAS waveform model for the dominant $(\ell, |m|) =$ (2,2) modes to eccentric binaries. For the inspiral part, orbit-averaged equations of motion within the quasi-Keplerian parametrization up to third post-Newtonian order, including spin effects, are evolved, and the waveform modes are computed using the stationary phase approximation on eccentricity expanded expressions up to $\mathcal{O}(e^{12})$. The model assumes circularization at merger-ringdown, where it adopts the underlying quasicircular IMRPhenomXAS baseline. We show that IMRPhenomXE reduces to the accurate IMPhenomXAS model in the quasi-circular limit. Compared against 186 public numerical relativity waveforms from the Simulating eXtreme Spacetimes catalog with initial eccentricities up to $~0.8$, IMRPhenomXE provides values of unfaithfulness below $3\%$ for $72\%$ of simulations with initial eccentricities below 0.4. For larger eccentricities, the unfaithfulness degrades up to $\gtrsim 10\%$ due to the underlying small eccentricity expansions and additional modelling approximations. In terms of speed, IMRPhenomXE outperforms any of the existing inspiral-merger-ringdown eccentric waveform models. We demonstrate the efficiency, robustness, and modularity of IMRPhenomXE through injections into zero noise and parameter-estimation analyses of gravitational-wave events, showing that IMRPhenomXE is a ready-to-use waveform model for gravitational-wave astronomy in the era of rapidly growing event catalogs.

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