标题： 一个后牛顿理论中的偏心双黑洞 显示英文标题

标题： An eccentric binary blackhole in post-Newtonian theory

摘要： 在双黑洞合并过程中辐射的引力波是研究强引力特征的完美探针。 用于创建数值相对论替代模型的先进技术，对于偏心双黑洞系统来说，在现有和预期的引力波探测器中被认为将变得更加关键。 由双黑洞合并产生的引力波观测数据中的痕迹增强了双体系统的研究。 本研究的目的是概述分层大质量天体合并特征行为的变化，这些数据是早期宇宙的数据库。 我们提供了在后牛顿框架下对等质量和非等质量无自旋吸积双黑洞系统的数值相对论模拟结果。 我们还考虑了初始偏心系统的偏心率的时间演化。 偏心后牛顿方程以与频率相关的变量$x = (M \omega)^{2/3}$的形式展开。 该模型仅限于 (2, 2) 自旋加权球面调和模式。 我们得出结论，对于更高的偏心率以及质量比，轨道半径和偏心率中存在更高的振荡。 显示英文摘要

摘要： Gravitational waves radiated during binary black hole coalescence is a perfect probe for studying the characteristics of strong gravity. Advanced techniques for creating numerical relativity substitute models for eccentric binary black hole systems are presumed to become more crucial in existing and anticipated gravitational wave detectors. The imprint on the observation data of the gravitational wave emitted by the binary coalescence enhances the two body system studies. The aim of this study is to present an overview of the change in characteristics behaviours of hierarchical massive astrophysical objects merger, which are the data bank of the early universe. We present results from numerical relativity simulations of equal-mass and unequal mass nonspinning inspiral binary-black-hole system in the Post Newtonian framework. We also consider the time evolution of eccentricity for the initial eccentric system. The eccentric Post Newtonian equations are expanded in the form of frequency related variable $x = (M \omega)^{2/3}$. The model is restricted to the (2, 2) spin-weighted spherical harmonic modes. We conclude that for higher eccentricity as well as mass ratio there exist higher oscillation in orbital radius and in eccentricity.