Probing a cosmological model with a = 0 + 3β H2 decaying-vacuum
Abstract
In this work we study the evolution of matter-density perturbations for an arbitrary (t) model, and specialize our analysis to the particular phenomenological law = 0 + 3β H2. We study the evolution of the cosmic star formation rate in this particular dark energy scenario and, by constraining the β parameter using both the age of the universe and the cosmic star formation rate curve, we show that it leads to a reasonable physical model for β 0.1.
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