Parametrized black hole quasinormal ringdown: Decoupled equations for nonrotating black holes
Parametrized black hole quasinormal ringdown: Decoupled equations for nonrotating black holes
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DOI：
10.1103/physrevd.99.104077
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发表时间：
2019-05-29
影响因子：
5
通讯作者：
McManus, Ryan
中科院分区：
文献类型：
--
作者：
Cardoso, Vitor;Kimura, Masashi;McManus, Ryan
广义相对论中的黑洞解很简单。这些解周围的线性扰动的频谱（即，准正规模）也很简单，因此它是黑洞时空和引力基础理论的基本测试的主要目标。为了理解任何修正的引力理论在光谱上的印记，必须进行以下技术计算：1。一个健康的理论; 2。在理论中找到黑洞解; 3.计算黑洞时空的线性化扰动方程; 4.求解这些方程以计算特征准简正模。在这篇文章（系列文章的第一篇）中，我们假设背景时空具有球对称性，相关的物理学总是接近广义相对论，并且微扰方程之间没有耦合。在这些假设下，我们提供了步骤4的一般数值解。我们提供了公开可用的数据文件，使得任何球对称时空的准正规模可以计算（原则上）到任意精度，一旦线性化微扰方程是已知的。我们证明了偶宇称和奇宇称准正规模谱之间的等谱性是脆弱的，并确定了保持等谱性的必要条件。最后，我们指出，即使在微扰接近广义相对论的情况下，谱中也会出现新的模。
Black hole solutions in general relativity are simple. The frequency spectrum of linear perturbations around these solutions (i.e., the quasinormal modes) is also simple, and therefore it is a prime target for fundamental tests of black hole spacetimes and of the underlying theory of gravity. The following technical calculations must be performed to understand the imprints of any modified gravity theory on the spectrum: 1. Identify a healthy theory; 2. Find black hole solutions within the theory; 3. Compute the equations governing linearized perturbations around the black hole spacetime; 4. Solve these equations to compute the characteristic quasi normal modes. In this work (the first of a series) we assume that the background spacetime has spherical symmetry, that the relevant physics is always close to general relativity, and that there is no coupling between the perturbation equations. Under these assumptions, we provide the general numerical solution to step 4. We provide publicly available data files such that the quasi normal modes of any spherically symmetric spacetime can be computed (in principle) to arbitrary precision once the linearized perturbation equations are known. We show that the isospectrality between the even- and odd-parity quasinormal mode spectra is fragile, and we identify the necessary conditions to preserve it. Finally, we point out that new modes can appear in the spectrum even in setups that are perturbatively close to general relativity.