Radial oscillations and stability of compact stars in $f(R, T) = R+ 2\beta T$ gravity

TL;DR

This paper investigates the structure and stability of compact stars in a modified gravity theory, deriving new equations and analyzing how stellar properties are affected by the $f(R, T)$ gravity model.

Contribution

It introduces the hydrostatic equilibrium and pulsation equations for $f(R, T)$ gravity and confirms that classical stability criteria remain valid in this framework.

Findings

Mass-radius relations are computed for various equations of state.

Stability conditions $dM/d ho_c >0$ and $ ext{omega}^2 >0$ are confirmed to hold.

Radial mode frequencies are obtained and analyzed.

Abstract

We examine the static structure configurations and radial stability of compact stars within the context of $f(R, T)$ gravity, with $R$ and $T$ standing for the Ricci scalar and trace of the energy-momentum tensor, respectively. Considering the $f(R, T)=R+2\beta T$ functional form, with $\beta$ being a constant, we derive the corresponding hydrostatic equilibrium equation and the modified Chandrasekhar's pulsation equation. The mass-radius relations and radial mode frequencies are obtained for some realistic equations of state. Our results show that the traditional stellar stability criteria, namely, the necessary condition $dM/d\rho_c >0$ and sufficient condition $\omega^2 >0$, still hold in this theory of gravity.