BINARY BLACK HOLE MERGER IN GALACTIC NUCLEI: POST-NEWTONIAN SIMULATIONS
BINARY BLACK HOLE MERGER IN GALACTIC NUCLEI: POST-NEWTONIAN SIMULATIONS
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DOI：
10.1088/0004-637x/695/1/455
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发表时间：
2008-12
期刊：
影响因子：
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通讯作者：
I. Berentzen;Miguel Preto;P. Berczik;D. Merritt;R. Spurzem
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文献类型：
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作者：
I. Berentzen;Miguel Preto;P. Berczik;D. Merritt;R. Spurzem
本文研究旋转星系核中双超大质量黑洞（SMBH）的形成和演化，重点关注恒星动力学的作用。我们提出了第一个 N 体模拟，该模拟跟踪了超大质量黑洞从千秒差距分离一直到最终相对论合并的演变，并且可以稳健地扩展到真实星系。 N 体代码包括对高达 2.5 阶的二元运动方程的后牛顿修正；我们证明，只有包含保守项和项，才能正确再现大规模二进制文件的演化。在我们的模拟中，经常发现大质量双星的轨道偏心率一直很大，直到合并前不久。这不仅直接影响它们的轨道演化速率，而且对相对论螺旋期间发出的引力波形也产生重要影响。当频率落在（计划的）激光干涉仪空间天线（LISA）频带内时，我们估计引力波振幅。我们发现高次谐波的显着贡献（远高于 LISA 灵敏度曲线）。
This paper studies the formation and evolution of binary supermassive black holes (SMBHs) in rotating galactic nuclei, focusing on the role of stellar dynamics. We present the first N-body simulations that follow the evolution of the SMBHs from kiloparsec separations all the way to their final relativistic coalescence, and that can robustly be scaled to real galaxies. The N-body code includes post-Newtonian corrections to the binary equations of motion up to order 2.5; we show that the evolution of the massive binary is only correctly reproduced if the conservative and terms are included. The orbital eccentricities of the massive binaries in our simulations are often found to remain large until shortly before coalescence. This directly affects not only their orbital evolution rates, but has important consequences as well for the gravitational waveforms emitted during the relativistic inspiral. We estimate gravitational wave amplitudes when the frequencies fall inside the band of the (planned) Laser Interferometer Space Antennae (LISA). We find significant contributions—well above the LISA sensitivity curve—from the higher-order harmonics.