亚pc尺度下大质量黑洞双星高偏心率的起源和意义
Origin and Implications of high eccentricities in massive black hole binaries at sub-pc scales
摘要：
本文概述了星系合并过程中形成的亚秒差距大质量黑洞双星的偏心率演化。在恒星和气体环境中，MBHB在进入引力波（GW）观测领域之前，预计会增长较大的轨道偏心率。我们重新访问预测的偏心率检测的空间激光干涉仪（作为拟议的ELISA/NGO）的两种环境。接近聚结时，许多MBHB仍将保持可检测的离心率，范围从<10^{-5}到<~ 0.5。恒星和气体驱动的动力学导致不同的分布，后者有利于更大的偏心率。在较大的二元分离，当发射的GWs将被观测到脉冲星定时阵列（PTA），预期的偏心率通常是相当大的，在0.01-0.7的范围内，这对信号建模和检测算法提出了一个重要的问题。在这个窗口中，大偏心率也有建议的电磁对应的GW信号，我们简要回顾的影响。
英文摘要：
We outline the eccentricity evolution of sub-parsec massive black hole binaries (MBHBs) forming in galaxy mergers. In both stellar and gaseous environments, MBHBs are expected to grow large orbital eccentricities before they enter the gravitational wave (GW) observational domain. We re--visit the predicted eccentricities detectable by space based laser interferometers (as the proposed ELISA/NGO) for both environments. Close to coalescence, many MBHBs will still maintain detectable eccentricities, spanning a broad range from <10^{-5} up to <~ 0.5. Stellar and gas driven dynamics lead to distinct distributions, with the latter favoring larger eccentricities. At larger binary separations, when emitted GWs will be observed by pulsar timing arrays (PTAs), the expected eccentricities are usually quite large, in the range 0.01-0.7, which poses an important issue for signal modelling and detection algorithms. In this window, large eccentricities also have implications on proposed electromagnetic counterparts to the GW signal, which we briefly review.
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