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I am not an expert on the matter of inhomogeneous cosmology, but in view of the above discussion it is interesting to check the latest developments here:
What is called inhomogeneous cosmology is the study of cosmology via cosmological solutions to Einstein's equations, whithout assuming or constraining these solutions to be spatially homogeneous (in the technical sense).
This is in contrast to the standard model of cosmology, based on FRW model-type solutions to Einstein's equations, where spacetime is assumed to be spatially homogeneous.
Of course the observable universe is clearly not exactly homogeneous, but the question is whether on cosmic scales the deviation from homogeneity is small enough that it may be neglected, to first approximation, for the purpose of modelling cosmological evolution.
The standard model of cosmology assumes that this is the case, and studies structure formation as a perturbation about a homogeneous background spacetime.
Given that the standard model of cosmology faces some issues related to dark energy/cosmological constant (and possibly related issues such as cosmic inflation or dark matter), it has been suggested that these may be but an artifact of the overly idealistic approximation of cosmic homogeneity, and that a more accurate inhomogeneous cosmology would not need to assume any dark energy (e.g. Buchert 07, Buchert 11, Buchert-Rasanen 11, also Scharf 13).
A seminal argument that it is consistent to neglect cosmic inhomogeneity due to (Green-Wald 10, Green-Wald 13), has been called into question in Buchert et al. 15, where it is concluded that the question is more subtle and remains open. Recent review is in Belejko-Korzyński 16.
What is called inhomogeneous cosmology is the study of cosmology via cosmological solutions to Einstein's equations, whithout assuming or constraining these solutions to be spatially homogeneous (in the technical sense).
This is in contrast to the standard model of cosmology, based on FRW model-type solutions to Einstein's equations, where spacetime is assumed to be spatially homogeneous.
Of course the observable universe is clearly not exactly homogeneous, but the question is whether on cosmic scales the deviation from homogeneity is small enough that it may be neglected, to first approximation, for the purpose of modelling cosmological evolution.
The standard model of cosmology assumes that this is the case, and studies structure formation as a perturbation about a homogeneous background spacetime.
Given that the standard model of cosmology faces some issues related to dark energy/cosmological constant (and possibly related issues such as cosmic inflation or dark matter), it has been suggested that these may be but an artifact of the overly idealistic approximation of cosmic homogeneity, and that a more accurate inhomogeneous cosmology would not need to assume any dark energy (e.g. Buchert 07, Buchert 11, Buchert-Rasanen 11, also Scharf 13).
A seminal argument that it is consistent to neglect cosmic inhomogeneity due to (Green-Wald 10, Green-Wald 13), has been called into question in Buchert et al. 15, where it is concluded that the question is more subtle and remains open. Recent review is in Belejko-Korzyński 16.