Cauchy-horizon singularity inside perturbed Kerr black holes
Cauchy-horizon singularity inside perturbed Kerr black holes
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扰动克尔黑洞内的柯西视界奇点
DOI：
10.1103/physrevd.93.041501
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发表时间：
2016
影响因子：
5
通讯作者：
Anil Zenginovglu
中科院分区：
文献类型：
--
作者：
L. Burko;G. Khanna;Anil Zenginovglu
一个奇点在每个黑洞（BH）内部演化，正如霍金-彭罗斯奇点定理在非常合理的条件下所保证的那样。相对而言，人们对BH奇点的性质知之甚少，包括它们的物理和几何性质，时空流形延伸到它们之外的可能性，或者量子引力所扮演的角色。基于球形玩具模型和宇宙学奇点的性质，以及对旋转黑洞的微扰和非微扰分析，人们相信在现实黑洞内部可能存在三种类型的奇点，并且可能共存：第一，Belinskiii-Khalatnikov-Lifshitz型奇点[2]，一个类空的、各向异性的、均匀的和混沌的奇点，其中Kasner历元独立地沿沿着不同的类时途径交替出现;第二，Poisson-Israel质量暴胀奇点[3]，沿着BH的Cauchy视界的生成元或进入内视界演化的一个无形变的弱奇点，第三，Marolf-Ori奇点[4]，一种零激波奇点，由于捕获了过去的扰动，它沿着向外的内视界的发生器演化。在这里，我们主要关注的是旋转黑洞内部的质量膨胀奇点，特别是奇点在早期部分的性质。在文献[5]中，对球形带电标量场玩具模型的质量暴胀奇异性进行了全非线性模拟，证实了其一般特征的性质。然而，微扰分析[6]预测的质量暴胀奇点特征的几个关键细节似乎与[5]的非线性结果不一致。这种差异通过参考文献[7]的仔细模拟得到了解决，它表明在质量暴胀奇点微扰的早期部分，
A singularity evolves inside every black hole (BH), as guaranteed under very plausible conditions by the Hawking-Penrose singularity theorems [1]. Relatively little is known about the nature of BH singularities, including their physical and geometrical properties, the possibility of extension of the spacetime manifold beyond them, or the role played by quantum gravity. Based on properties of spherical toy models and of cosmological singularities in addition to perturbative and nonperturbative analysis of rotating BHs, it is believed that three types of singularitiescould exist, and possiblycoexist, inside realistic BHs: first, a Belinskii-Khalatnikov-Lifshitztype singularity [2], a spacelike, anisotropic, homogeneous and chaotic singularity, in which Kasner epochs alternate independently along different timelike approaches to the singularity; second, the Poisson-Israel mass-inflation singularity[3],anullanddeformationallyweaksingularitythat evolvesalongthegeneratorsoftheBH’sCauchyhorizon,or ingoing inner horizon, because of the capture of future perturbations; and third, the Marolf-Ori singularity [4] ,a null shock-wave singularity that evolves along the generators of the outgoinginner horizonbecauseof the capture of past perturbations. Here we are mostly concerned with the mass-inflation singularity inside rotating BHs, and specifically with the properties of the singularity in its early parts. The massinflation singularity was simulated in fully nonlinear simulations for a spherical charged scalar-field toy model in Ref. [5], where the properties of its general features were confirmed. However, several key details of the features of the mass-inflation singularity that were predicted by perturbative analysis [6] appeared to be inconsistent with the nonlinear results of [5]. This discrepancy was resolved by the careful simulations of Ref. [7], which showed that in the early parts of the mass-inflation singularity perturbation