Conservation Laws for Cosmological Perurbations

TL;DR

This paper discusses the definition of conserved quantities like energy in cosmological models, applying a formalism to perturbed Robertson-Walker spacetimes with de Sitter backgrounds and relating results to integral constraints in cosmology.

Contribution

It introduces a formalism for defining conserved quantities in perturbed cosmological spacetimes and connects these to existing integral constraints, with applications in cosmology.

Findings

Conserved quantities can be defined using a symmetric background in perturbed spacetimes.

The formalism relates to Traschen's integral constraints.

Applications include insights into energy conservation in cosmological perturbations.

Abstract

We briefly recall the problem of defining conserved quantities such as energy in general relativity, and the solution by introducing a symmetric background. We apply the general formalism to perturbed Robertson-Walker spacetimes with de Sitter geometry as background. We relate the obtained conserved quantities to Traschen's integral constraints and mention a few applications in cosmology.