Growth of Perturbations in Tsallis and Barrow Cosmology

TL;DR

This paper investigates how entropic corrections from Tsallis and Barrow entropies modify the Friedmann equations and influence the growth rate of cosmological perturbations in the early universe.

Contribution

It introduces modified Friedmann equations based on Tsallis and Barrow entropies and analyzes their impact on the growth of matter perturbations in a flat universe.

Findings

Density contrast profiles differ from standard cosmology.

Growth rate of perturbations depends on Tsallis and Barrow parameters.

Perturbations grow faster with increasing entropy correction parameters.

Abstract

We disclose the effects of the entropic corrections to the Friedmann equations on the growth of perturbations in the early stages of the universe. We consider two types of corrections to the area law of entropy, known as Tsallis and Barrow entropies. Using these corrections to entropy, we derive the modified Friedmann equations and explore the growth of perturbations in a flat universe filled with dark matter (DM) and cosmological constant. We employ the spherically symmetric collapse formalism and work in the linear regime for the perturbations. Interestingly enough, we find out that the profile of density contrast quite differs from the standard cosmology in Tsallis and barrow cosmology. We observe that the growth rate of matter perturbations crucially depend on the values of Tsallis and Barrow parameters. With increasing these correction parameters to the entropy, the total density contrast increases as well. This implies that perturbations grow up faster in a universe with modified entropy corrected Friedmann equations.