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Dark energy and dissipation

By Diego Pavón, Luis P. Chimento and Ro S. Jakubi

Abstract

Most of the models leading to a current state of cosmic accelerated expansion fail to address the coincidence problem, i.e., that the dark energy density and the energy density of the matter fluid are of the same order precisely today. We show that a way to drive late acceleration and simultaneously solve the aforesaid problem is assuming the matter fluid dissipative [1]. 1 General setting The Friedmann equation plus the conservation equations for matter and dark energy in a Friedmann–Robertson–Walker universe dominated by these two components (non–interacting with one another), in terms of the density parameters, rea

Year: 2008
OAI identifier: oai:CiteSeerX.psu:10.1.1.317.4596
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