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

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.

Automated summary

In this study, the static structure configurations and radial stability of compact stars were examined within the context of f(R, T) gravity. The mass-radius relations and radial mode frequencies were obtained for some realistic equations of state. The results showed that the traditional stellar stability criteria still hold in this theory of gravity.