Effects of Charge and Gravitational Decoupling on Complexity and Isotropization of Anisotropic Models

TL;DR

This study explores how charge and gravitational decoupling influence the complexity and isotropization of anisotropic stellar models within Einstein-Maxwell theory, providing extended solutions and analyzing their physical viability.

Contribution

It introduces a method to extend anisotropic solutions using minimal geometric deformation and decoupling parameters, offering new models for charged, anisotropic compact stars.

Findings

Models are physically acceptable for most parameter values.

Charge and decoupling parameters affect star properties.

Solutions are graphically interpreted for a specific compact star.

Abstract

This paper constructs two immediate extensions of the existing anisotropic solutions in the context of Einstein-Maxwell framework by employing minimal geometric deformation. To achieve this, we assume a static spherical interior initially filled with anisotropic fluid and call it a seed source. We extend this matter configuration by including a new source whose impact on the self-gravitating system is governed by a decoupling parameter. The charged field equations analogous to the total fluid source are formulated. We then implement a transformation on the radial metric potential that divides the field equations into two new under-determined systems, corresponding to the initial and new sources. The first of them is addressed by taking two well-known metric ansatz so that the number of unknowns can be tackled. Further, the vanishing of total anisotropy and complexity-free constraints are used to solve the second set. The estimated radius and mass of a compact star $4U~1820-30$ is utilized to interpret the resulting solutions graphically for different values of the charge and decoupling parameter $\omega$. We conclude that our both developed models are physically acceptable for all parametric values except $\omega=1$.