Analytic Black Hole Perturbation Approach to Gravitational Radiation.
Analytic Black Hole Perturbation Approach to Gravitational Radiation.
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DOI：
10.12942/lrr-2003-6
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发表时间：
2003
影响因子：
40.6
通讯作者：
Tagoshi H
中科院分区：
文献类型：
--
作者：
Sasaki M;Tagoshi H
本文回顾了基于黑洞微扰理论的后牛顿引力波展开的解析方法。存在两种不同的方法来执行后牛顿展开。两者都是基于Teukolsky方程。在一种方法中，Teukolsky方程被转换成Regge-Wheeler型方程，在平坦空间极限中简化为标准的Klein Gordon方程，而在另一种方法中（由Mano，Suzuki和Takasugi相对较新地引入），Teukolsky方程直接以其原始形式使用。前者的优点是直观上容易理解各种弯曲空间效果是如何发挥作用的。然而，当人们进入越来越高的后牛顿阶时，它变得越来越复杂。相比之下，后者的优点是可以相对容易地实现更高后牛顿阶的系统计算，但除此之外，它是如此数学化，以至于很难理解高阶项的相互作用。在本文中，我们回顾这两种方法，使他们的优点和缺点可能会清楚地看到。我们还回顾了一些计算结果的引力辐射的粒子轨道黑洞。
We review the analytic methods used to perform the post-Newtonian expansion of gravitational waves induced by a particle orbiting a massive, compact body, based on black hole perturbation theory. There exist two different methods of performing the post-Newtonian expansion. Both are based on the Teukolsky equation. In one method, the Teukolsky equation is transformed into a Regge-Wheeler type equation that reduces to the standard Klein Gordon equation in the flat-space limit, while in the other method (which was introduced by Mano, Suzuki, and Takasugi relatively recently, the Teukolsky equation is used directly in its original form. The former’s advantage is that it is intuitively easy to understand how various curved space effects come into play. However, it becomes increasingly complicated when one goes to higher and higher post-Newtonian orders. In contrast, the latter’s advantage is that a systematic calculation to higher post-Newtonian orders can be implemented relatively easily, but otherwise, it is so mathematical that it is hard to understand the interplay of higher order terms. In this paper, we review both methods so that their pros and cons may be seen clearly. We also review some results of calculations of gravitational radiation emitted by a particle orbiting a black hole.