Quasilocal Energy in FRW Cosmology

Abstract

This paper presents a calculation of the quasilocal energy of a generic FRW model of the universe. The results have the correct behavior in the small-sphere limit and vanish for the empty Milne universe. Higher order corrections are found when comparing these results to classical calculations of cosmological energy. This case is different from others in the literature chiefly in that it involves a non-stationary spacetime. This fact can be used to differentiate between the various formulations of quasilocal energy. In particular, the formulation due to Brown and York is compared to that of Epp. Only one of these is seen to have the correct classical limit.

The article has been revised for publication in Classical and Quantum Gravity. All calculations remain unchanged. A discussion of Epp's formulation and additional references have been added

References in corpus (3)

• Positivity of Quasilocal Mass
• Isometric embeddings into the Minkowski space and new quasi-local mass
• Gravitational energy and cosmic acceleration

Cited by in corpus (7)

• Cosmic structure, averaging and dark energy
• Intrinsic vanishing of energy and momenta in a universe
• Optimal Choices of Reference for a Quasi-local Energy: Spherically Symmetric Spacetimes
• Quasilocal conservation laws in cosmology: a first look
• Energy of cosmological spacetimes and perturbations: a quasilocal approach
• Energy in critical collapse
• Note on the Conservation of Quasi-Local Energy in an Expanding Universe