Anisotropic Compact Stellar Objects in Modified Gauss-Bonnet Gravity

TL;DR

This study models anisotropic compact stars within modified Gauss-Bonnet gravity, demonstrating their viability and stability through analytical and graphical analysis of physical conditions.

Contribution

It introduces a new approach using embedding class-1 technique in modified Gauss-Bonnet gravity to analyze anisotropic stellar structures and their stability.

Findings

Models are viable and stable for observed compact stars.

Predicted radii match observational data.

Solution satisfies physical and stability conditions.

Abstract

This paper is devoted to studying anisotropic compact stellar structures by adopting embedding class-1 technique in the background of modified Gauss-Bonnet gravity. The unknown constants are evaluated by the matching of interior spacetime with the Schwarzschild exterior geometry corresponding to $f(\mathcal{G})=\chi\mathcal{G}^{n}$ model, where $\chi$ and $n$ are positive constants. The observed masses of compact star candidates (SAX J1808.4-3658, Vela X-1, PSR J0348+0432, 4U 1608-52) are used with the condition of vanishing radial pressure at the stellar surface to predict their radii. We have examined viability and stability of the resulting solution through graphical behavior of matter variables, energy constraints, adiabatic index and causality condition. It is found that embedding class-1 solution for anisotropic compact stars is viable and stable in this theory.