Transition from decelerated to accelerated cosmic expansion in braneworld universes

TLDR: In this article, the authors focused their attention on models where the vacuum energy decreases as an inverse power law of the scale factor, which is consistent with the observed accelerating universe, while fitting simultaneously the observational data for the density and deceleration parameter.

Abstract: Braneworld theory provides a natural setting to treat, at a classical level, the cosmological effects of vacuum energy. Non-static extra dimensions can generally lead to a variable vacuum energy, which in turn may explain the present accelerated cosmic expansion. We concentrate our attention in models where the vacuum energy decreases as an inverse power law of the scale factor. These models agree with the observed accelerating universe, while fitting simultaneously the observational data for the density and deceleration parameter. The redshift at which the vacuum energy can start to dominate depends on the mass density of ordinary matter. For $$\bar \Omega$$ m = 0.3, the transition from decelerated to accelerated cosmic expansion occurs at z T ≈ 0.48 ± 0.20, which is compatible with SNe data. We set a lower bound on the deceleration parameter today, namely $$\bar{q}$$ > − 1 + 3 $$\bar \Omega$$ m /2, i.e., $$\bar{q}$$ > − 0.55 for $$\bar \Omega $$ m = 0.3. The future evolution of the universe crucially depends on the time when vacuum starts to dominate over ordinary matter. If it dominates only recently, at an epoch z 0.64, then the deceleration comes back and the universe recollapses at some point in the distant future. In the first case, quintessence and Cardassian expansion can be formally interpreted as the low energy limit of our model, although they are entirely different in philosophy. In the second case there is no correspondence between these models and ours.