Abstract
Quintessential inflation assumes a common origin for inflation and the dark energy of the Universe. In this scenario reheating can occur through gravitational particle production during the inflation-kination transition. We provide a detailed study of gravitational reheating in quintessential inflation and determine the temperature T* at which radiation starts dominating over kination, generalizing previous analyses only available for the standard case when inflation is followed by an era dominated by the energy density of radiation, The value of T* is controlled by the Hubble parameter H0 during inflation and the transition time Δt, scaling as H02 [ln(1/H0Δt)]3/4 for H0Δt ≪ 1 and H02(H0Δt)−c for H0t ≫ 1. The model-dependent parameter c is found to be around 0.5 in two different parametrizations for the transition between inflation and kination.
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