Back-Reaction in Relativistic Cosmology
Abstract
We introduce the concept of back-reaction in relativistic cosmological modeling. Roughly speaking, this can be thought of as the difference between the large-scale behaviour of an inhomogeneous cosmological solution of Einstein's equations, and a homogeneous and isotropic solution that is a best-fit to either the average of observables or dynamics in the inhomogeneous solution. This is sometimes paraphrased as `the effect that structure has of the large-scale evolution of the universe'. Various different approaches have been taken in the literature in order to try and understand back-reaction in cosmology. We provide a brief and critical summary of some of them, highlighting recent progress that has been made in each case.
Keywords
Cite
@article{arxiv.1302.6717,
title = {Back-Reaction in Relativistic Cosmology},
author = {Timothy Clifton},
journal= {arXiv preprint arXiv:1302.6717},
year = {2015}
}
Comments
13 pages, 2 figures. Based on a talk given at the 13th Marcel Grossmann meeting