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Effect of inhomogeneities on the expansion rate of the Universe
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While the expansion rate of a homogeneous isotropic Universe is simply proportional to the square-root of the energy density, the expansion rate of an inhomogeneous Universe also depends on the nature of the density inhomogeneities. In this paper we calculate to second order in perturbation variables the expansion rate of an inhomogeneous Universe and demonstrate corrections to the evolution of the expansion rate. While we find that the mean correction is small, the variance of the correction on the scale of the Hubble radius is sensitive to the physical significance of the unknown spectrum of density perturbations beyond the Hubble radius.
Forward citations
Cited by 2 Pith papers
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Back-reaction of cosmological inhomogeneities can make an effective dark energy with a time-dependent equation of state and no phantom crossing, even for a global average.
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Full Einstein-Vlasov simulations show Newtonian N-body collapse is faster than general relativity for extreme density perturbations, but accurate at subpercent level for standard cosmological amplitudes.
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