Abstract

Within the quantum mechanical treatment of the decay problem one finds that at late times tthe survival probability of an unstable state cannot have the form of an exponentially decreasing function of time t but it has an inverse power-like form. This is a general property of unstable states following from basic principles of quantum theory. The consequence of this property is that in the case of false vacuum states the cosmological constant becomes dependent on time: Λ — Λbare ≡ Λ(t) — Λbare ∼ 1/t2. We construct the cosmological model with decaying vacuum energy density and matter for solving the cosmological constant problem and the coincidence problem. We show the equivalence of the proposed decaying false vacuum cosmology with the Λ(t) cosmologies (the Λ(t)CDM models). The cosmological implications of the model of decaying vacuum energy (dark energy) are discussed. We constrain the parameters of the model with decaying vacuum using astronomical data. For this aim we use the observation of distant supernovae of type Ia, measurements of H(z), BAO, CMB and others. The model analyzed is in good agreement with observation data and explain a small value of the cosmological constant today.

Highlights

  • The most natural explanation of the acceleration of the Universe seems to be the cosmological constant param eter interpreted as vacuum energy

  • A lthough such an explanation is simple it brings a conundrum th at the values of the cosmological constant required by quantum theory ( ~ 1071 GeV4) and obtained from ty p e Ia supernovae observations

  • (v) The cosmological models w ith decaying vacuum be can treated as an extension of the doi:10.1088/1742-6596/626/1/012033

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Summary

Introduction

The most natural explanation of the acceleration of the Universe seems to be the cosmological constant param eter interpreted as vacuum energy. O ur idea is to derive th e p aram etrization of decaying vacuum energy directly from th e first principle, namely from the quantum mechanics, to construct the cosmological model and to test it statistically using astronom ical d ata. For estim ation of the model param eters we assume th a t

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