Complete waveform model for compact binaries on eccentric orbits
E. A. Huerta, Prayush Kumar, Bhanu Agarwal, Daniel George, Hsi-Yu Schive, Harald P. Pfeiffer, Roland Haas, Wei Ren, Tony Chu, Michael Boyle, Daniel A. Hemberger… 展开作者
E. A. Huerta, Prayush Kumar, Bhanu Agarwal, Daniel George, Hsi-Yu Schive, Harald P. Pfeiffer, Roland Haas, Wei Ren, Tony Chu, Michael Boyle, Daniel A. Hemberger, Lawrence E. Kidder, Mark A. Scheel, Bela Szilagyi
备注：
31 pages, 19 figures, 3 appendices. Submitted to Phys Rev D. v2: direct comparison to eccentric numerical relativity simulations, not used for calibration of the model, included. References added. Accepted to Phys Rev D
We present a time domain waveform model that describes the inspiral-merger-ringdown (IMR) of compact binary systems whose components are non-spinning, and which evolve on orbits with low to moderate eccentricity. The inspiral evolution is described using third order post-Newtonian equations both for the equations of motion of the binary, and its far-zone radiation field. This latter component also includes instantaneous, tails and tails-of-tails contributions, and a contribution due to non-linear memory. This framework reduces to the post-Newtonian approximant TaylorT4 at third post-Newtonian order in the zero eccentricity limit. To improve phase accuracy, we incorporate higher-order post-Newtonian corrections for the energy flux of quasi-circular binaries and gravitational self-force corrections to the binding energy of compact binaries. This enhanced inspiral evolution prescription is combined with an analytical prescription for the merger-ringdown evolution using a catalog of numerical relativity simulations. This IMR waveform model reproduces effective-one-body waveforms for systems with mass-ratios between 1 to 15 in the zero eccentricity limit. Using a set of eccentric numerical relativity simulations, not used during calibration, we show that our eccentric model accurately reproduces the features of eccentric compact binary coalescence throughout the merger. Using this model we show that the gravitational wave transients GW150914 and GW151226 can be effectively recovered with template banks of quasi-circular, spin-aligned waveforms if the eccentricity $e_0$ of these systems when they enter the aLIGO band at a gravitational wave frequency of 14 Hz satisfies $e_0^{\rm GW150914}\leq0.15$ and $e_0^{\rm GW151226}\leq0.1$.
Stochastic Gravitational Wave Background from Highly-Eccentric Stellar-Mass Binaries in the Milli-hertz Band
UCLA（加州大学洛杉矶分校）；Mani L. Bhaumik Institute for Theoretical Physics, Department of Physics and Astronomy, UCLA（加州大学洛杉矶分校物理与天文学系马尼·L·巴乌米克理论物理研究所）；Rudolf Peierls Centre for Theoretical Physics, Parks Road, Oxford（牛津大学鲁道夫·派尔斯理论物理中心）
Revisiting the Coprecessing Frame in the Presence of Orbital Eccentricity
California Institute of Technology（加州理工学院）；LIGO Laboratory, California Institute of Technology（LIGO实验室，加州理工学院）；Department of Physics & Astronomy, Amherst College（阿默斯特学院物理与天文系）；Cornell Center for Astrophysics and Planetary Science, Cornell University（康奈尔大学天体物理学与行星科学中心）
ESIGMAHM: An Eccentric, Spinning inspiral-merger-ringdown waveform model with Higher Modes for the detection and characterization of binary black holes
Pulsar timing array signals induced by black hole binaries in relativistic eccentric orbits
非圆轨道上的单个超大质量黑洞双星可能是快速成熟的脉冲星定时阵列实验的纳赫兹引力波源。我们发展了一种精确有效的方法来计算脉冲星定时阵列信号，由于引力波从吸入相对论偏心轨道的超大质量黑洞双星。我们的方法采用开普勒型参数解模型的第三后牛顿精确进动偏心轨道，而一个新的半解析处方提供了模型的四极阶引力波发射的影响。这些输入导致一个半解析的处方来模拟这样的信号，引起的非自旋黑洞二进制沿任意偏心率轨道螺旋。此外，我们提供了一个完整的分析处方模型脉冲星定时阵列信号从黑洞二进制沿适度偏心轨道吸气，Boetzelet等人的影响。[Phys. Rev. D 96，044011（2017）]。这些方法正在被纳入企业和TEMPO 2搜索脉冲星定时阵列数据集中存在这样的二进制文件。
Adding higher-order spherical harmonics in non-spinning eccentric binary black hole merger waveform models
Kavli Institute for Theoretical Physics, University of California Santa Barbara（加州大学圣塔芭芭拉分校卡弗里理论物理研究所）；Theoretical AstroPhysics Including Relativity and Cosmology, California Institute of Technology（加利福尼亚理工学院包括相对论和宇宙学的理论天体物理学）；Department of Physics and Center for Computational Research, University of Rhode Island（罗德岛大学物理系与计算研究中心）；Department of Physics, University of Massachusetts, Dartmouth（麻省大学达特茅斯分校物理系）；Center for Scientific Computing and Data Science Research, University of Massachusetts, Dartmouth（麻省大学达特茅斯分校科学计算与数据科学研究中心）；Department of Mathematics, University of Massachusetts, Dartmouth（麻省大学达特茅斯分校数学系）
High accuracy post-Newtonian and numerical relativity comparisons involving higher modes for eccentric binary black holes and a dominant mode eccentric inspiral-merger-ringdown model
Adding eccentricity to quasicircular binary-black-hole waveform models
从合并偏心双星黑洞的引力波信号的检测将产生前所未有的信息，在特定的情况下，如致密的星团和三体相互作用的动力学形成的致密双星的形成和演化。地面干涉仪LIGO和Virgo的引力波搜索依赖于准圆轨道上双星的分析波形模型。偏心合并的波形模型发展较少，只有少数的偏心合并的数值模拟是公开的，但几个偏心inspiral模型已经开发出后牛顿膨胀。在这里，我们提出了一种新的方法来转换的主导四极模式的任何圆形的分析双黑洞模型到偏心模型。首先，使用数值模拟，我们研究的额外的振幅和频率调制的偏心信号，不存在于他们的圆形同行。随后，我们确定了这些调制的合适的分析描述，并从指定为我们的训练数据集的12个数值模拟中插入关键参数。这使我们能够重建质量比为3和偏心率为0.2的任何波形的调制幅度和相位。我们发现，新模型与数值模拟的最小重叠约为0.98，在我们所有的测试数据集上，这些数据集以35 Hz的频率从aLIGO A+设计灵敏度开始缩放到50 M $_\odot$黑洞二进制。一个Python包\pyrex可以很容易地执行这种方法的计算。
Data-driven extraction, phenomenology and modeling of eccentric harmonics in binary black hole merger waveforms
Kavli Institute for Theoretical Physics, University of California Santa Barbara（加州大学圣塔芭芭拉分校卡弗里理论物理研究所）；Theoretical AstroPhysics Including Relativity and Cosmology, California Institute of Technology（加州理工学院理论天体物理学（含相对论与宇宙学））；Department of Physics, University of California at Santa Barbara（加州大学圣塔芭芭拉分校物理系）；International Centre for Theoretical Sciences, Tata Institute of Fundamental Research（印度塔塔基础研究院国际理论科学中心）；Department of Physics and Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学物理与天文系）；School of Natural Sciences, Institute for Advanced Study（普林斯顿高等研究院自然科学院）；TAPIR, Walter Burke Institute for Theoretical Physics, California Institute of Technology（加州理工学院沃尔特·伯克理论物理研究所 TAPIR）；Department of Particle Physics & Astrophysics, Weizmann Institute of Science（魏茨曼科学研究所粒子物理与天体物理系）
