Effect of Extended Gravitational Decoupling on Isotropization and Complexity in f(\mathbb{R},\mathbb{T}) Theory

TL;DR

This study introduces new analytical solutions in extended gravitational decoupling within $f(R,T)$ gravity, demonstrating how specific parameters influence isotropization, complexity, and stability of compact star models.

Contribution

It develops novel analytical solutions in $f(R,T)$ gravity using extended gravitational decoupling, focusing on isotropization and complexity reduction in stellar models.

Findings

Certain parameter values produce viable, stable star solutions.

The models achieve isotropization at specific decoupling parameters.

Complexity-free configurations are attainable within the framework.

Abstract

This paper develops some new analytical solutions to the $f(\mathbb{R},\mathbb{T})$ field equations through extended gravitational decoupling. For this purpose, we take spherical anisotropic configuration as a seed source and extend it to an additional source. The modified field equations comprise the impact of both sources which are then decoupled into two distinct sets by applying the transformations on $g_{tt}$ and $g_{rr}$ metric potentials. The original anisotropic source is adorned by the first sector, and we make it solvable by considering two different well-behaved solutions. The second sector is in terms of an additional source and we adopt some constraints to find deformation functions. The first constraint is the isotropization condition which transforms the total fluid distribution into an isotropic system only for a specific value of the decoupling parameter. The other constraint is taken as the complexity-free fluid distribution. The unknown constants are calculated at the hypersurface through matching conditions. The preliminary information (mass and radius) of a compact star $4U 1820-30$ is employed to analyze physical attributes of the resulting models. We conclude that certain values of both the coupling as well as decoupling parameter yield viable and stable solutions in this theory.