Finch-Skea star model in f(R, T ) theory of gravity

TL;DR

This paper develops a compact star model within $f(R,T)$ gravity using the Finch-Skea ansatz, analyzing its physical properties and stability for the pulsar PSR J1614-2230.

Contribution

It introduces a new compact star model in $f(R,T)$ gravity with explicit solutions and stability analysis based on the Finch-Skea ansatz.

Findings

Model is physically consistent and stable.

Geometry and matter are compatible.

Applicable to real pulsar data.

Abstract

The present work discusses about the existence of compact star model in the context of $f(R,T)$ gravity with $R$ as the Ricci scalar and $T$ as the trace of energy-momentum tensor $T_{\mu \nu}$. The model has been developed by considering the spherically symmetric spacetime consisting of isotropic fluid with $f(R,T)=R+2 \beta T$ with $\beta$ be the coupling parameter. The corresponding field equations are solved by choosing well known Finch-Skea {\em ansatz} [Finch, M.R., Skea, J.E.F.:{\it Class. Quantum Gravity} {\bf 6}, 467 (1989)]. For spacetime continuity we elaborate the boundary conditions by considering the exterior region as Schwarzschild metric. The unknown constants appearing in the solution are evaluated for the compact star PSR~J 1614-2230 for different values of coupling constant. The physical properties of the model, e.g., matter density, pressure, stability etc. have been discussed both analytically and graphically. This analysis showed that the geometry and matter are compatible with each other as well as the model is in stable equilibrium in the context of $f(R,\,T)$ modified gravity.