发表机构
Max Planck Institute for Gravitational Physics (Albert Einstein Institute); Nottingham Centre of Gravity & School of Mathematical Sciences, University of Nottingham; Department of Physics, University of Maryland; Cornell Center for Astrophysics and Planetary Science, Cornell University; Departament de Física, Universitat de les Illes Balears（马克斯·普朗克引力物理研究所（爱因斯坦研究所）; 诺丁汉大学重力中心与数学科学学院; 马里兰大学物理系; 康奈尔大学天体物理学与行星科学中心; 巴利阿里群岛大学物理系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究提出SEOBNRv6EPHM模型，可精准高效分析任意轨道自旋进动双黑洞的引力波，提升偏心分析精度与速度，为引力波天文学提供了新工具。
AI 中文摘要
在致密恒星环境或层级三体系统中形成的双黑洞（BBH）可在偏心轨道并合，且具有任意取向的自旋，会在其引力波（GW）辐射上留下独特印记。我们提出SEOBNRv6EPHM：这是自2011年以来支撑LIGO-Virgo引力波分析的有效单天体SEOBNR系列中首个任意轨道、自旋进动模型，其波形可描述任意轨道双黑洞的动力学及多极引力波信号，涵盖并合双星的旋进-并合-铃荡阶段，并延伸至动力学捕获和散射遭遇过程。我们针对自旋进动双黑洞的数值相对论（NR）波形，开展了首个任意轨道模型的系统性精度评估，使用1437个准圆（QC）模拟和87个偏心模拟：中位数波形失配保持在1%以下，与准圆模型SEOBNRv5PHM的精度相当，且较当前最先进的任意轨道模型TEOBResumS-Dalí提升了4倍的中位数水平。该模型还能重现任意自旋双黑洞散射的数值相对论模拟中观测到的非微扰现象学。在准圆极限下，其速度约为SEOBNRv5PHM的2-3倍，且比TEOBResumS-Dalí快一个数量级，使偏心分析的成本降至当前准圆分析的水平。作为原理验证，我们分析了11个引力波事件，重点关注GW200129，强化了其偏心的证据——该结果得到了偏心、自旋进动双黑洞的合成数值相对论信号的注入-恢复研究支持。因此，SEOBNRv6EPHM首次实现了同时考虑偏心和自旋进动的精准高效引力波分析。
英文摘要
Binary black holes (BBHs) formed in dense stellar environments or in hierarchical triples can coalesce on eccentric orbits and carry spins of arbitrary orientation, leaving distinctive imprints on their gravitational-wave (GW) emission. We present SEOBNRv6EPHM: the first generic-orbit, spin-precessing model in the effective-one-body SEOBNR family, whose waveforms have underpinned LIGO-Virgo GW analyses since 2011. The model describes the dynamics and multipolar GW signal of generic BBHs, covering the inspiral-merger-ringdown of coalescing binaries and extending to dynamical captures and scattering encounters. We perform the first systematic accuracy assessment of a generic-orbit model against numerical relativity (NR) waveforms of spin-precessing BBHs, using 1437 quasi-circular (QC) and 87 eccentric simulations: median waveform mismatches remain below $1 \%$, matching the accuracy of the QC model SEOBNRv5PHM, and improving on the state-of-the-art generic-orbit model TEOBResumS-Dalí by a median factor of $ 4 $. The model also reproduces the non-perturbative phenomenology observed in NR simulations of generic-spin BBH scattering. It is $\sim 2 - 3$ times faster than SEOBNRv5PHM in the QC limit, and up to an order of magnitude faster than TEOBResumS-Dalí, bringing eccentric inference to the cost of current QC analyses. As a proof of principle, we analyze eleven GW events and focus on GW200129, strengthening its evidence for eccentricity $-$ a result supported by injection-recovery studies with synthetic NR signals of eccentric, spin-precessing BBHs. SEOBNRv6EPHM thus enables, for the first time, accurate and efficient GW analyses that jointly account for eccentricity and spin precession.
Comments26 pages, 12 figures
