Compact Stars in $f(\mathcal{R,G,T})$ Gravity

TL;DR

This paper introduces a new modified gravity theory, $f( ext{R,G,T})$, and explores its implications for the physical features, stability, and structure of relativistic compact stars, including detailed analysis of specific star models.

Contribution

The work develops the field equations and physical analysis framework for $f( ext{R,G,T})$ gravity, applying it to model and examine compact stars with novel insights.

Findings

Energy conditions are satisfied in the models.

Compact stars have dense cores.

Stability and equilibrium conditions are confirmed.

Abstract

The present work is to introduce a new kind of modified gravitational theory, named as $f(\mathcal{R,G,T})$ (also $f(\mathcal{R,T,G})$) gravity, where $\mathcal{R}$ is the Ricci scalar, $\mathcal{G}$ is Gauss-Bonnet invariant and $\mathcal{T}$ is the trace of the energy-momentum tensor. With the help of different models in this gravity, we investigate some physical features of different relativistic compact stars. For this purpose, we develop the effectively modified field equations, conservation equation, and the equation of motion for test particle. Then, we check the impact of additional force (massive test particle followed by a non-geodesic line of geometry) on compact objects. Furthermore, we took three notable stars named as $Her X-1$, $SAXJ1808.4-3658$ and $4U1820-30$. The physical behavior of the energy density, anisotropic pressures, different energy conditions, stability, anisotropy, and the equilibrium scenario of these strange compact stars are analyzed through various plots. Finally, we conclude that the energy conditions hold, and the core of these stars is so dense.