Tolman IV fluid sphere in f(R, T) gravity

TL;DR

This paper explores the structure of relativistic compact stars within f(R, T) gravity using Tolman IV spacetime, analyzing how the coupling parameter affects physical properties and ensuring the model's physical viability.

Contribution

It presents a new stellar model in f(R, T) gravity with a detailed analysis of the coupling parameter's effects on star properties, ensuring physical consistency.

Findings

Higher coupling parameter increases sound speed and adiabatic index.

Mass function decreases with higher coupling parameter.

Model satisfies all physical conditions for realistic stars.

Abstract

In this article, we studied the behavior of relativistic spherical objects considering Tolman IV spacetime in modified $f(R,\,T)$ gravity for the uncharged perfect fluid matter. We have chosen the matter Lagrangian as $\mathcal{L}_m=-p$ to develop our present model. In particular, for this investigation we have reported for the compact object LMC $X-4$ [Mass=$(1.04 \pm 0.09)M_{\odot}$; Radius= $8.301_{-0.2}^{+0.2}$ Km] in our paper. The effect of the coupling parameter $\beta$ on the local matter distribution of compact stars has been investigated in this paper. It can be seen that with greater values of $\beta$, the sound speed and adiabatic index are higher. On contrary, the mass function takes lower value for higher values of $\beta$. Our obtained solution does not admit singularities in the matter density, pressure and metric functions. According to our graphical analysis, this new stellar model satisfies all physical requirements anticipated in a realistic star.