arXiv 1707.080562017-07gr-qcastro-ph.CO

黑洞宇宙结构形成的准静态方法

A Quasi-Static Approach to Structure Formation in Black Hole Universes

Jessie Durk, Timothy Clifton

备注：: 33 pages, 10 figures, v2: matches published version, typos corrected
发表信息：: JCAP 10 (2017) 012

摘要：

受宇宙结构层次结构存在的启发，我们提出了四个新的非均匀宇宙学模型在其最大膨胀时的精确初始数据族。这些数据概括了现有的黑洞晶格模型的情况下，包含集群的质量，因此允许宇宙学结构的后果被认为是在一个明确的和非微扰的方式。聚集的程度由参数$λ$控制，对于$λ\sim 0$或$1$，我们有非常紧密的聚集质量，而对于$λ\sim 0.5$，所有质量都由宇宙学距离尺度分开。我们研究的后果，在我们的每个集群的总净质量的结构形成，以及计算的相互作用能量内和集群之间的宇宙学后果。当一组黑洞足够靠近时，它们周围出现的共享视界的位置也被确定和研究。我们发现，集群可以对宇宙学的规模有惊人的大的影响，与模型，包含数千个黑洞有时是小到30%的规模可比弗里德曼模型具有相同的总固有质量。这种缺陷与弗里德曼宇宙学中忽略引力相互作用能所预期的结果相当，并表明这些量可能对大尺度宇宙学的性质产生重大影响。

英文摘要：

Motivated by the existence of hierarchies of structure in the Universe, we present four new families of exact initial data for inhomogeneous cosmological models at their maximum of expansion. These data generalise existing black hole lattice models to situations that contain clusters of masses, and hence allow the consequences of cosmological structures to be considered in a well-defined and non-perturbative fashion. The degree of clustering is controlled by a parameter $λ$, in such a way that for $λ\sim 0$ or $1$ we have very tightly clustered masses, whilst for $λ\sim 0.5$ all masses are separated by cosmological distance scales. We study the consequences of structure formation on the total net mass in each of our clusters, as well as calculating the cosmological consequences of the interaction energies both within and between clusters. The locations of the shared horizons that appear around groups of black holes, when they are brought sufficiently close together, are also identified and studied. We find that clustering can have surprisingly large effects on the scale of the cosmology, with models that contain thousands of black holes sometimes being as little as 30% of the size of comparable Friedmann models with the same total proper mass. This deficit is comparable to what might be expected to occur from neglecting gravitational interaction energies in Friedmann cosmology, and suggests that these quantities may have a significant influence on the properties of the large-scale cosmology.

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