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首页> 外文期刊>Physical review, D >Parametrized black hole quasinormal ringdown: Decoupled equations for nonrotating black holes
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Parametrized black hole quasinormal ringdown: Decoupled equations for nonrotating black holes

机译：参数化的黑洞准法线衰减：非旋转黑洞的解耦方程

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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 quasinormal 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 quasinormal 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.
机译：广义相对论中的黑洞解决方案很简单。这些解周围的线性摄动的频谱（即准正交模式）也很简单，因此，它是黑洞时空基础理论和引力理论的主要目标。为了理解任何修正的重力理论在频谱上的影响，必须进行以下技术计算：1.确定健康的理论; 2.在理论内找到黑洞的解; 3.计算控制黑洞时空周围线性化摄动的方程; 4.求解这些方程式以计算特征准正规模。在这项工作（系列的第一个）中，我们假设背景时空具有球对称性，相关物理总是接近于广义相对论，并且摄动方程之间没有耦合。在这些假设下，我们提供了第4步的一般数值解。我们提供了可公开获得的数据文件，以便一旦知道线性化摄动方程，就可以（原则上）以任意精度计算任何球对称时空的准正态模。 。我们证明了偶校验和奇校验准准模谱之间的等光谱是脆弱的，并且我们确定了保留它的必要条件。最后，我们指出，即使在与广义相对论非常接近的设置中，新模式也会出现在频谱中。

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