Gravitational backreaction in cosmological spacetimes

TL;DR

This paper introduces a novel formalism for analyzing gravitational backreaction in cosmological spacetimes, employing group-averaging techniques to derive effective equations that account for inhomogeneities and their potential to cause accelerated cosmic expansion.

Contribution

It develops a new group-averaging based formalism for gravitational backreaction, providing effective equations for inhomogeneous cosmologies and exploring conditions for acceleration.

Findings

Effective backreaction equations derived for dust-filled spacetimes.

Identification of conditions leading to cosmic acceleration due to inhomogeneities.

Analysis of regimes with small and large inhomogeneities in gravitational backreaction.

Abstract

We develop a new formalism for the treatment of gravitational backreaction in the cosmological setting. The approach is inspired by projective techniques in non-equilibrium statistical mechanics. We employ group-averaging with respect to the action of the isotropy group of homogeneous and isotropic spacetimes (rather than spatial averaging), in order to define effective FRW variables for a generic spacetime. Using the Hamiltonian formalism for gravitating perfect fluids, we obtain a set of equations for the evolution of the effective variables; these equations incorporate the effects of backreaction by the inhomogeneities. Specializing to dust-filled spacetimes, we find regimes that lead to a closed set of backreaction equations, which we solve for small inhomogeneities. We then study the case of large inhomogeneities in relation to the proposal that backreaction can lead to accelerated expansion. In particular, we identify regions of the gravitational state space that correspond to effective cosmic acceleration. Necessary conditions are (i) a strong expansion of the congruences corresponding to comoving observers, and (ii) a large negative value of a dissipation variable that appears in the effective equations (i.e, an effective "anti-dissipation").