Deflation of the cosmological constant associated with inflation and dark energy

Abstract

In order to solve the fine-tuning problem of the cosmological constant, we propose a simple model with the vacuum energy non-minimally coupled to the inflaton field. In this model, the vacuum energy decays to the inflaton during pre-inflation and inflation eras, so that the cosmological constant effectively deflates from the Planck mass scale to a much smaller one after inflation and plays the role of dark energy in the late-time of the universe. We show that our deflationary scenario is applicable to arbitrary slow-roll inflation models. We also take two specific inflation potentials to illustrate our results.

12 pages, 5 figures, revised version accepted by JCAP

References in corpus (7)

• Dynamics of dark energy
• Cosmologies with Energy Exchange
• Unification of inflation and dark energy {\it à la} quintessential inflation
• Evolution of density perturbations in decaying vacuum cosmology
• Coupled quintessence and vacuum decay
• Observational constraints on varying neutrino-mass cosmology
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Cited by in corpus (3)

• Constraints on running vacuum model with $H(z)$ and $f{\sigma }_8$
• Matter density perturbation and power spectrum in running vacuum model
• Deflation of Vacuum Energy During Inflation Due to Bulk-Brane Interaction