论文标题
牛顿后理论中的古怪二进制黑洞
An eccentric binary blackhole in post-Newtonian theory
论文作者
论文摘要
在二进制黑洞合并期间辐射的重力波是研究强重力特征的理想探针。假定在现有和预期的引力波检测器中，推定用于创建用于偏心二进制黑洞系统的数值相对替代模型的高级技术变得更加重要。二元聚结发出的重力波的观察数据的烙印增强了两个身体系统的研究。这项研究的目的是概述层次大规模天体物理对象合并的特征行为的变化，即早期宇宙的数据库。我们通过在牛顿后框架中对等质量和不等质量的非灵感二进制二进制黑洞系统的数值相对性模拟的结果提出了结果。我们还考虑了初始偏心系统偏心率的时间演变。偏心的牛顿方程以相关变量的形式扩展，$ x =（mΩ）^{2/3} $。该模型仅限于（2，2）自旋加权球形谐波模式。我们得出的结论是，对于较高的偏心率和质量比，轨道半径和偏心率的振荡较高。
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 $x = (M ω)^{2/3}$. 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.
