The Kerr-de Sitter universe
The Kerr-de Sitter universe
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DOI：
10.1088/0264-9381/28/8/085012
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发表时间：
2011-04-21
影响因子：
3.5
通讯作者：
Matzner, Richard A.
中科院分区：
文献类型：
--
作者：
Akcay, Sarp;Matzner, Richard A.
现在人们普遍认为，我们所理解的宇宙正在加速膨胀，并且非常符合德西特模型。因此，对黑洞的现实假设必须将它们置于德西特背景上，而不是像广义相对论中通常所做的那样置于闵可夫斯基背景上。与天体物理学最相关的黑洞是不带电的旋转克尔解，它是更通用的克尔-纽曼度量的成员。 Carter 发现了将旋转克尔黑洞推广到具有宇宙学常数 Lambda 的爱因斯坦方程解的方法（1973 Les Astres Occlus ed B DeWitt 和 C M DeWitt（纽约：Gordon and Breach））。它通常被称为克尔德西特时空。在这里，我们讨论这个时空的视界结构及其对 Lambda 的依赖。我们记得，在 Lambda > 0 宇宙中，术语“极值黑洞”是指角动量 J > M-2 的黑洞。我们获得了黑洞最大自旋值的显式数值结果，并获得了（Lambda，自旋）参数空间中可接受的克尔空穴的分布。我们研究扩展时空的共形结构和空间超曲面的 3 几何形状的嵌入。与 Reissner-Nordstrom-de Sitter 时空类比，特别是通过将 Kerr-de Sitter 因果结构视为 Reissner-Nordstrom-de Sitter 因果结构的扭曲，我们证明扩展时空的空间部分是 3 球体，其中包含极点处克尔空洞视界的二维拓扑球形部分。根据 t = 常数 3 空间的定义方式，这些孔可能被视为黑洞或白孔（四种可能的组合）。
It is now widely accepted that the universe as we understand it is accelerating in expansion and fits the de Sitter model rather well. As such, a realistic assumption of black holes must place them on a de Sitter background and not Minkowski as is typically done in general relativity. The most astrophysically relevant black hole is the uncharged, rotating Kerr solution, a member of the more general Kerr-Newman metrics. A generalization of the rotating Kerr black hole to a solution of the Einstein's equation with a cosmological constant Lambda was discovered by Carter (1973 Les Astres Occlus ed B DeWitt and C M DeWitt (New York: Gordon and Breach)). It is typically referred to as the Kerrde Sitter spacetime. Here, we discuss the horizon structure of this spacetime and its dependence on Lambda. We recall that in a Lambda > 0 universe, the term 'extremal black hole' refers to a black hole with angular momentum J > M-2. We obtain explicit numerical results for the black hole's maximal spin value and get a distribution of admissible Kerr holes in the (Lambda, spin) parameter space. We look at the conformal structure of the extended spacetime and the embedding of the 3-geometry of the spatial hypersurfaces. In analogy with Reissner-Nordstrom-de Sitter spacetime, in particular by considering the Kerr-de Sitter causal structure as a distortion of the Reissner-Nordstrom-de Sitter one, we show that spatial sections of the extended spacetime are 3-spheres containing two-dimensional topologically spherical sections of the horizons of Kerr holes at the poles. Depending on how a t = constant 3-space is defined, these holes may be seen as black or white holes (four possible combinations).