LIGO-Virgo-KAGRA合作组织使用的有效单体（EOB）波形，主要是通过对相对论两体问题的后牛顿展开进行重求和而发展起来的。鉴于近期在后闵可夫斯基（PM）理论和引力自力形式方面取得的重大进展，人们对于构建以创新方式整合来自各种微扰方法信息的波形模型产生了浓厚兴趣。在应对未来十年内预期运行的下一代地基探测器（如Einstein Telescope和Cosmic Explorer）以及天基探测器（如LISA、TianQin或Taiji）所带来的精度挑战时，这一点尤为关键。在此背景下，我们推导了首个包含最高至三圈阶PM结果的自旋EOB哈密顿量：SEOB-PM模型。该模型考虑了完整的双曲运动，包括时间非局域尾效应。为了评估其准确性，我们将其对保守散射角的预测（并附加了耗散贡献）与非自旋和自旋等质量黑洞的数值相对论数据进行了比较。我们观察到非常好的一致性，其表现与最近提出的$w_{\ m EOB}$势模型相当，在某些情况下甚至略优于该模型；而SEOB-PM模型正是围绕试探质量极限对该势模型的一种重求和。事实上，在试探质量极限下，SEOB-PM哈密顿量和散射角会退化为Kerr时空中测试粒子的对应结果。一旦补充了束缚轨道的时间非局域贡献，SEOB-PM哈密顿量即可用于生成准圆轨道上自旋黑洞的波形模型。
英文摘要：
Effective-one-body (EOB) waveforms employed by the LIGO-Virgo-KAGRA Collaboration have primarily been developed by resumming the post-Newtonian expansion of the relativistic two-body problem. Given the recent significant advancements in post-Minkowskian (PM) theory and gravitational self-force formalism, there is considerable interest in creating waveform models that integrate information from various perturbative methods in innovative ways. This becomes particularly crucial when tackling the accuracy challenge posed by upcoming ground-based detectors (such as the Einstein Telescope and Cosmic Explorer) and space-based detectors (such as LISA, TianQin or Taiji) expected to operate in the next decade. In this context, we present the derivation of the first spinning EOB Hamiltonian that incorporates PM results up to three-loop order: the SEOB-PM model. The model accounts for the complete hyperbolic motion, encompassing nonlocal-in-time tails. To evaluate its accuracy, we compare its predictions for the conservative scattering angle, augmented with dissipative contributions, against numerical-relativity data of non-spinning and spinning equal-mass black holes. We observe very good agreement, comparable, and in some cases slightly better to the recently proposed $w_{\rm EOB}$-potential model, of which the SEOB-PM model is a resummation around the probe limit. Indeed, in the probe limit, the SEOB-PM Hamiltonian and scattering angles reduce to the one of a test mass in Kerr spacetime. Once complemented with nonlocal-in-time contributions for bound orbits, the SEOB-PM Hamiltonian can be utilized to generate waveform models for spinning black holes on quasi-circular orbits.
Resumming Spinning Black Hole Dynamics at Third Post-Minkowskian Order
Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Niels Bohr International Academy, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所尼尔斯·玻尔国际学院）
Scattering angle at 3PM in scalar-tensor theories using the PM-EFT formalism
Laboratoire d’étude de l’Univers et des phénomènes eXtrêmes (LUX), Observatoire de Paris, Université PSL, Sorbonne Université, CNRS（极端宇宙与现象研究实验室，巴黎天文台，巴黎文理研究大学，索邦大学）；LPENS, Département de physique, Ecole normale supérieure, Université PSL, Sorbonne Université, Université Paris Cité, CNRS（物理与环境理论物理研究所，巴黎高等师范学院，巴黎文理研究大学，索邦大学，巴黎西岱大学）；Observatoire de Paris, Université PSL, Sorbonne Université, CNRS（巴黎天文台，巴黎文理研究大学，索邦大学）
Unexpected Symmetries of Kerr Black Hole Scattering
Higgs Centre for Theoretical Physics, School of Physics and Astronomy, University of Edinburgh（爱丁堡大学物理与天文学学院希格斯理论物理中心）；Centre for Theoretical Physics, Department of Physics and Astronomy, Queen Mary University of London（伦敦玛丽女王大学物理与天文学院理论物理中心）
Radiated Angular Momentum from Spinning Black Hole Scattering Trajectories
Humboldt-Universität zu Berlin（柏林洪堡大学）；Max Planck Institut für Gravitationsphysik (Albert Einstein Institut)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Queen Mary University of London（伦敦玛丽女王大学）
A novel Lagrange-multiplier approach to the effective-one-body dynamics of binary systems in post-Minkowskian gravity
Institut des Hautes Etudes Scientifiques（高等科学研究所）；INFN Sezione di Torino（都灵国家核物理研究所）；Dipartimento di Fisica e Geologia, Università di Perugia（佩鲁贾大学物理与地质学系）；INFN Sezione di Perugia（佩鲁贾国家核物理研究所）
Spinning Black Hole Scattering at $\mathcal{O}(G^3 S^2)$: Casimir Terms, Radial Action and Hidden Symmetry
University of Edinburgh（爱丁堡大学）；Florida State University（佛罗里达州立大学）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）；University of California at Los Angeles（加州大学洛杉矶分校）
Black Hole Thermodynamics Meets On-Shell Amplitudes: Local Detailed Balance and Thermal Spectrum from Spin Universality and Unitarity
Centre for Mathematical Sciences, Plymouth University（普利茅斯大学数学科学中心）；Higgs Centre for Theoretical Physics, School of Physics and Astronomy, University of Edinburgh（爱丁堡大学物理与天文学学院希格斯理论物理中心）；Graduate School of Science and Engineering, Saitama University（埼玉大学理工学研究科）；Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University（京都大学汤川理论物理中心引力物理与量子信息研究中心）；Department of Physics, Graduate School of Science, The University of Tokyo（东京大学理学研究科物理学系）；Research Center for the Early Universe (RESCEU), Graduate School of Science, The University of Tokyo（东京大学理学研究科宇宙早期宇宙研究中心）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学卡弗里宇宙起源研究所（世界顶级研究中心））；Graduate School of Arts and Sciences, University of Tokyo（东京大学大学院综合文化研究科）
