Comparison of 4.5PN and 2SF gravitational energy fluxes from quasicircular compact binaries
University College Dublin（都柏林大学学院）；CEICO, Institute of Physics of the Czech Academy of Sciences（捷克科学院物理研究所 CEICO）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理学研究所（爱因斯坦研究所））；University of Southampton（南安普顿大学）；Sorbonne Université（索邦大学）；CNRS（法国国家科学研究中心）；Institut d’Astrophysique de Paris（巴黎天体物理学研究所）；University of Texas at Austin（德克萨斯大学奥斯汀分校）；Shamoon College of Engineering（沙蒙工程学院）
Niels Warburton, Barry Wardell, David Trestini, Quentin Henry, Adam Pound, Luc Blanchet, Leanne Durkan, Guillaume Faye, Jeremy Miller
备注：
18 pages, 6 figures, modes of PN flux provided in ancillary file, v2: major update due to corrections to the self-force data, v3: matches published version
Recent years have seen significant advances in models of gravitational waveforms emitted by quasicircular compact binaries in two regimes: the weak-field, post-Newtonian regime, in which the gravitational wave energy flux has now been calculated to fourth-and-a-half post-Newtonian order (4.5PN) [Phys. Rev. Lett. 131}, 121402 (2023)]; and the small-mass-ratio, gravitational self-force regime, in which the flux has now been calculated to second perturbative order in the mass ratio (2SF) [Phys. Rev. Lett. 127, 151102 (2021)]. We compare these results and find evidence of mutual consistency between the two (very distinct though both first-principle) perturbative calculations.
Quadrupole and quadratic-in-spin effects in quasicircular, spinning, asymmetric binaries
Kyoto University（京都大学）；Astronomical Institute of the Czech Academy of Sciences（捷克科学院天文研究所）；University of Southampton（南安普顿大学）；National University of Singapore（新加坡国立大学）
Effective-one-body waveforms for extreme-mass-ratio binaries: Consistency with second-order gravitational self-force quasicircular results and extension to nonprecessing spins and eccentricity
Asymptotic frame selection for binary black hole spacetimes II: Post-Newtonian limit
从引力辐射中选择一个优选坐标系的一种方法是< L L>通过旋转群生成元在渐近无穷远处对外尔张量作用的平均值的主轴。在本文中，我们评估这个时域平均准圆二进制使用近似（后牛顿）波形。对于非旋进不等质量双星，我们表明这个张量的主导特征向量位于沿轨道角动量。对于旋进双星，这个坐标系通常与轨道或总角动量不一致，在自旋中起主导作用。这两个量之间的差异随着时间的推移而增长，因为二进制接近螺旋的末端，岁差和更高的谐波变得更加重要。
Adiabatic evolution of asymmetric binaries on generic orbits with new fundamental fields I: characterization of gravitational wave fluxes
Gran Sasso Science Institute (GSSI)（格兰萨索科学研究所）；INFN, Laboratori Nazionali del Gran Sasso（意大利国家核物理研究所，格兰萨索国家实验室）；Dipartimento di Fisica, Sapienza Università di Roma（罗马智慧大学物理系）；Dipartimento di Fisica, Università di Pisa（比萨大学物理系）；INFN, Sezione di Roma（意大利国家核物理研究所罗马分部）；School of Mathematics and Statistics, University College Dublin（都柏林大学学院数学与统计学院）；INFN, Sezione di Pisa（意大利国家核物理研究所比萨分部）；School of Mathematical Sciences & School of Physics and Astronomy, University of Nottingham（诺丁汉大学数学科学学院与物理与天文学院）；Nottingham Centre of Gravity, University of Nottingham（诺丁汉大学引力研究中心）
Gravitational waves from inspiralling compact binaries: Angular momentum flux, evolution of the orbital elements and the wave form to the second post-Newtonian order
Waveforms and fluxes: Towards a self-consistent effective one body waveform model for nonprecessing, coalescing black-hole binaries for third generation detectors
Enhancing the SEOBNRv5 effective-one-body waveform model with second-order gravitational self-force fluxes
Niels Bohr International Academy, Niels Bohr Institute（尼尔斯·玻尔国际学院，尼尔斯·玻尔研究所）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Department of Physics, University of Maryland（马里兰大学物理系）；School of Mathematics and Statistics, University College Dublin（都柏林大学学院数学与统计学院）；School of Mathematical Sciences and STAG Research Centre, University of Southampton（南安普顿大学数学科学学院及STAG研究中心）
Anomalies in the gravitational recoil of eccentric black-hole mergers with unequal mass ratios
线性动量的辐射对合并中的黑洞双星系统的质心产生反冲（或“反冲”）。最近的数值相对论计算表明，对于自旋位于轨道平面内的等质量自旋双星（“超级反冲”配置），偏心率可导致反冲速度增加约25%[U Sperhake et al. Phys. Rev. D 101（2020）024044（arXiv：1910.01598）]。在这里，我们调查的非零偏心的非自旋，不等质量的黑洞双星的反冲幅度和引力波发射的影响。我们证实，非零的偏心率在合并可能会导致更大的踢高达25%的准圆形的情况下。我们还发现，反冲速度$v$有一个振荡的偏心率的依赖关系，我们解释为合并时的落入方向和远心点（或近心点）方向之间的角度变化的结果。
High-accuracy drivers to simulate black hole binaries beyond general relativity with the fixing-the-equations approach
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Cornell University（康奈尔大学）；California State University Fullerton（加州州立大学富勒顿分校）；Perimeter Institute for Theoretical Physics（理论物理前沿研究所）；California Institute of Technology（加州理工学院）
Post-Newtonian dynamics of charged compact binaries
International Centre for Theoretical Physics Asia-Pacific, University of Chinese Academy of Sciences（国际理论物理中心亚太区，中国科学院大学）；Taiji Laboratory for GW Universe, University of Chinese Academy of Sciences（引力波宇宙太极实验室，中国科学院大学）；School of Physics and Optoelectronic Engineering, Yangtze University（长江大学物理与光电工程学院）；School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences（中国科学院大学杭州高等研究院基础科学与数学学院）；School of Physical Sciences, University of Chinese Academy of Sciences（中国科学院大学物理科学学院）；School of Physical Science and Technology, Lanzhou University（兰州大学物理科学与技术学院）；Institute of Theoretical Physics, Chinese Academy of Sciences（中国科学院理论物理研究所）
Waveform models for the gravitational-wave memory effect: III. Phenomenological frequency-domain model for nonspinning binaries
Laboratoire d’étude de l’Univers et des phénomènes eXtrêmes (LUX), Observatoire de Paris, Université PSL, Sorbonne Université, CNRS（极端宇宙现象实验室，巴黎天文台，巴黎文理研究大学，索邦大学，法国国家科学研究中心）；Department of Physics, University of Virginia（弗吉尼亚大学物理系）
From the confluent Heun equation to a new factorized and resummed gravitational waveform for circularized, nonspinning, compact binaries
Università di Roma Tor Vergata（罗马托尔维加塔大学）；INFN Sezione di Roma Tor Vergata（罗马托尔维加塔大学意大利国家核物理研究所分部）；INFN Sezione di Torino（都灵意大利国家核物理研究所分部）；Institut des Hautes Etudes Scientifiques（高等科学研究所）
