Quasi-Local Energy for Cosmological Models

Details Quasi-Local Energy for Cosmological Models Quasi-Local Energy for Cosmological Models

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008mgm..conf.2149n&link_type=abstract

"THE ELEVENTH MARCEL GROSSMANN MEETING On Recent Developments in Theoretical and Experimental General Relativity, Gravitation an

Mathematics

Logic

1

Quasi-Local Energy, Hamiltonian, Cosmology

Scientific paper

Our covariant Hamiltonian formalism gives a certain preferred Hamiltonian boundary term for quasi-local quantities which depends on the boundary conditions, plus a reference and displacement vector choice. With appropriate choices we found the quasi-local energy for the cosmological models. Homogeneous choices give vanishing energy for all regions of Bianchi class A models and positive energy for class B. Isotropic choices give energies proportional to the curvature parameter k: ie, vanishing for the flat case, positive for the closed model and negative(!) for the open model. Our values are consistent with the requirement that the energy vanishes for closed models. We have some conclusions regarding the best reference choice and two quasi-local desiderata: positivity and zero energy iff Minkowski space.

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