Baryogenesis in non-extensive Tsallis Cosmology

TL;DR

This paper explores how non-extensive Tsallis cosmology modifies early universe dynamics, enabling baryogenesis consistent with observations, and constrains the Tsallis parameter in agreement with quantum gravity predictions.

Contribution

It introduces a novel application of Tsallis Cosmology to baryogenesis, deriving modified Friedmann equations and constraining the Tsallis parameter based on observational data.

Findings

Tsallis corrections alter the Hubble function during radiation era

Modified density and pressure enable baryogenesis with standard interactions

The Tsallis parameter constraint aligns with quantum gravity GUP estimates

Abstract

Non-extensive Tsallis thermostatistics is a widespread paradigm to describe large-scale gravitational systems. In this work we use Tsallis Cosmology to study thermodynamic gravity and derive modified Friedmann equations. We show that corrections induced by non-extensivity affect the Hubble function evolution during the radiation-dominated epoch. In turn, this leads to non-trivial modifications of the mass density and pressure content of the Universe, which provide a viable mechanism allowing for baryogenesis, even in the presence of the standard interaction between the Ricci scalar and baryon current. By demanding consistency with current observational bounds on baryogenesis, we constrain Tsallis $\delta$ parameter to be $|\delta-1| \simeq 10^{-3}$. Based on the recently established connection between Tsallis thermostatistics and the quantum gravitational generalization of the uncertainty principle at Planck scale (GUP), we finally show that this bound is in agreement with the estimation of the GUP parameter predicted by many quantum gravity models.