Non-extensive Statistical Mechanics and the Thermodynamic Stability of FRW Universe

TL;DR

This paper explores the thermodynamic stability of the Friedmann-Robertson-Walker universe using non-extensive statistical mechanics, specifically Tsallis entropy and loop quantum gravity, to understand cosmic acceleration and stability constraints.

Contribution

It introduces a thermodynamic stability analysis of the FRW universe within non-extensive frameworks, deriving constraints and comparing results across models and black hole thermodynamics.

Findings

Heat capacity, free energy, and pressure are calculated for the models.

For Tsallis entropy, the parameter β is constrained between 1/2 and 2.

The universe's free energy must be negative for thermal equilibrium.

Abstract

In this article, we investigate the thermodynamic stability of the FRW universe for two examples, Tsallis entropy and loop quantum gravity, by considering non-extensive statistical mechanics. The heat capacity, free energy and pressure of the universe are obtained. For the Tsallis entropy model, we obtained the constraint for $\beta$, namely, $1/2 < \beta < 2$. The free energy of a thermal equilibrium universe must be less than zero. We suggest that the reason for the accelerated expansion of the universe is not due to Tsallis entropy. Similar results are obtained for loop quantum gravity. However, since the values of $\Lambda(\gamma)$ and $q$ cannot be determined in this model, the results become more subtle than that in the Tsallis entropy model. In addition, we compare the results for the universe with those for a Schwarzschild black hole.