Charged Anisotropic Tolman IV Solution in Matter-Geometry Coupled Theory

TL;DR

This paper explores charged anisotropic star models within a modified gravity framework, analyzing their physical properties and stability using observational data of quark stars, and finds that some models remain stable under these conditions.

Contribution

It introduces a charged anisotropic star model in $f( ext{R}, ext{T}, ext{Q})$ gravity using Tolman IV spacetime and a linear bag model equation of state, considering electromagnetic effects.

Findings

Her X-I and 4U 1820-30 are stable in the modified gravity model.

Charge and modified gravity corrections influence star properties.

Model viability depends on the coupling constant value.

Abstract

This paper discusses the interior distribution of several anisotropic star models coupled with an electromagnetic field in the context of $f(\mathcal{R},\mathcal{T},\mathcal{Q})$ gravity, where $\mathcal{Q}=\mathcal{R}_{\beta\xi}\mathcal{T}^{\beta\xi}$. In this regard, a standard model of this modified gravity is taken as $\mathcal{R}+\nu_{3}\mathcal{R}_{\beta\xi}\mathcal{T}^{\beta\xi}$, where $\nu_{3}$ symbolizes an arbitrary coupling constant. We assume a charged spherically symmetric metric that represents the interior geometry of compact quark stars and develop the corresponding modified field equations. These equations are then solved with the help of metric potentials of Tolman IV spacetime and a linear bag model equation of state. We consider the experimental data (i.e., radii and masses) of different quark models such as SMC X-4, SAX J 1808.4-3658, Her X-I and 4U 1820-30 to analyze how the charge and modified corrections affect their physical characteristics. The viability and stability of the resulting model is also checked for the considered star candidates with two different values of $\nu_{3}$. We conclude that only two models, Her X-I and 4U 1820-30 show stable behavior in this modified framework for both values of the coupling constant.