Energy Conditions in Extended $f(R,G,T)$ Gravity

TL;DR

This paper investigates the implications of extended $f(R,G,T)$ gravity on cosmic acceleration, analyzing specific models against energy conditions and observational parameters to understand potential future singularities.

Contribution

It introduces specific $f(R,G,T)$ models and assesses their viability using energy conditions and recent cosmological data.

Findings

Identifies conditions under which finite-time future singularities may occur.

Provides bounds on model parameters consistent with observational data.

Analyzes the impact of energy conditions on model viability.

Abstract

In this paper, we consider the flat Friedmann Lematre Robertson-Walke metric in the presence of perfect fluid models and extended $f(R,G,T)$ gravity (where $R$ is the Ricci scalar, $G$ is the Gauss Bonnet invariant and $T$ stands for trace of energy momentum tensor). In this context, we assume some specific realistic $f(R,G,T)$ models configuration that could be used to explore the finite-time future singularities that arise in late-time cosmic accelerating phases. In this scenario, we choose the most recent estimated values for the Hubble, deceleration, snap and jerk parameters to develop the viability and bounds on the models parameters induced by different energy conditions.