Inhomogeneous cosmology | Wikipedia audio article
Channel: wikipedia tts
Date: 08/12/2018

This is an audio version of the Wikipedia Article:
Inhomogeneous cosmology


00:01:17 1 Homogeneity
00:01:37 2 Perturbative approach
00:02:05 3 Non-perturbative approach
00:02:39 4 Exact solutions
00:03:18 5 Averaging methods



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SUMMARY
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In cosmology and general relativity, inhomogeneous cosmology in the most general sense (totally inhomogeneous universe) is modelling the universe as a whole with the spacetime which does not possess any spacetime symmetries. Typically considered cosmological spacetimes have either the maximal symmetry which composes of three translational symmetries and three rotational symmetries (homogeneity and isotropy with respect to every point of spacetime), the translational symmetry only (homogeneous models), or the rotational symmetry only (spherically symmetric models). Models with less symmetries (e.g. axisymmetric) are also considered as symmetric. However, it is common to call spherically symmetric models or non-homogeneous models as inhomogeneous. In inhomogeneous cosmology the large-scale structure of the universe is modelled by exact solutions of the Einstein field equations (i.e. non-perturbatively) unlike in the theory of cosmological perturbations which is the study of the Universe that takes structure formation (galaxies, galaxy clusters, the cosmic web) into account, but in a perturbative way.This usually includes the study of structure in the Universe by means of exact solutions of Einstein's field equations (i.e. metrics) or by spatial or spacetime averaging methods.