Quasilocal conservation laws in cosmology: a first look
Marius Oltean, Hossein Bazrafshan Moghaddam, Richard J. Epp
TL;DR
This paper explores the application of quasilocal stress-energy-momentum definitions, specifically the Brown-York tensor, to cosmology, providing initial computations for flat FLRW universes with perfect fluid matter.
Contribution
It introduces the use of Brown-York quasilocal stress-energy-momentum tensor in cosmology and presents initial calculations for flat FLRW models.
Findings
Computed the Brown-York tensor for flat FLRW spacetime.
Provided simple results demonstrating the tensor's application in cosmology.
Abstract
Quasilocal definitions of stress-energy-momentum---that is, in the form of boundary densities (in lieu of local volume densities)---have proven generally very useful in formulating and applying conservation laws in general relativity. In this essay, we take a first basic look into applying these to cosmology, specifically using the Brown-York quasilocal stress-energy-momentum tensor for matter and gravity combined. We compute this tensor and present some simple results for a flat FLRW spacetime with a perfect fluid matter source.
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