Non-singular inflation with vacuum decay

Abstract

On the basis of a semi-classical analysis of vacuum energy in an expanding spacetime, we describe a non-singular cosmological model in which the vacuum density decays with time, with a concomitant production of matter. During an infinitely long period we have an empty, inflationary universe, with H \approx 1. This primordial era ends in a fast phase transition, during which H and Λdecrease to nearly zero in a few Planck times, with release of a huge amount of radiation. The late-time scenario is similar to the standard model, with the radiation phase followed by a long dust era, which tends asymptotically to a de Sitter universe, with vacuum dominating again. An analysis of the redshift-distance relation for supernovas Ia leads to cosmological parameters in agreement with other current estimations.

Work presented at IRGAC 2006, Barcelona, July 11-15 2006. To appear in a special issue of Journal of Physics A

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• Evolution of density perturbations in decaying vacuum cosmology: The case of non-zero perturbations in the cosmological term
• CMB Temperature and Matter Power Spectrum in a Decay Vacuum Dark Energy Model
• Observational constraints on decaying vacuum dark energy model
• Relic gravitational waves in the frame of slow-roll inflation with a power-law potential and the detection