Stability of the Einstein static Universe in $f(R,T)$ gravity

TL;DR

This paper investigates the existence and stability of Einstein static universe solutions within $f(R,T)$ gravity, identifying conditions under which these solutions are stable and can support non-singular emergent cosmological models.

Contribution

It demonstrates that specific $f(R,T)$ models can admit stable Einstein static solutions, unlike in $f(R)$ gravity, and explores their role in emergent universe scenarios.

Findings

Two classes of solutions: one unstable saddle, one stable center.

Stable solutions can support non-singular emergent universe models.

Modifications in $f(R,T)$) gravity enable stable solutions absent in $f(R)$ gravity.

Abstract

The Einstein static (ES) universe has played a major role in various emergent scenarios recently proposed in order to cure the problem of initial singularity of the standard model of cosmology. In the herein model, we study the existence and stability of ES universe in the context of $f(R,T)$ modified theories of gravity. Considering specific forms of $f(R,T)$ function, we seek for the existence of solutions representing ES state. Using dynamical system techniques along with numerical analysis, we find two classes of solutions: the first one is always unstable of the saddle type while the second is always stable so that its dynamical behavior corresponds to a center equilibrium point. The importance of the second class of solutions is due to the significant duty they have in constructing non-singular emergent models in which the universe could have experienced past-eternally, a series of infinite oscillations about such an initial static state after which, it enters through a suitable physical mechanism, to an inflationary era. Considering specific forms for the functionality of $f(R,T)$, we show that this theory is capable of providing cosmological solutions which admit emergent universe (EU) scenarios. We also investigate homogeneous scalar perturbations for the mentioned models. The stability regions of the solutions are parametrized by a linear equation of state (EoS) parameter and other free parameters that will be introduced for the models. Our results suggest that modifications in $f(R,T)$ gravity would lead to stable solutions which are unstable in $f(R)$ gravity model.