Quasi-local energy for cosmological models

TL;DR

This paper applies a covariant Hamiltonian approach to compute quasi-local energy in cosmological models, revealing discrepancies with some established criteria and emphasizing the importance of boundary conditions and reference choices.

Contribution

It introduces a covariant Hamiltonian formalism for quasi-local energy and applies it to Bianchi and FRW cosmologies, highlighting differences with traditional criteria.

Findings

Quasi-local energies depend on boundary conditions and reference configurations.

Results differ from some widely accepted quasi-local criteria.

The formalism provides a new perspective on energy in cosmological models.

Abstract

First we briefly review our covariant Hamiltonian approach to quasi-local energy, noting that the Hamiltonian-boundary-term quasi-local energy expressions depend on the chosen boundary conditions and reference configuration. Then we present the quasi-local energy values resulting from the formalism applied to homogeneous Bianchi cosmologies. Finally we consider the quasi-local energies of the FRW cosmologies. Our results do not agree with certain widely accepted quasi-local criteria.