Stellar structure of quark stars in a modified Starobinsky gravity

Abstract

We propose a form of gravity-matter interaction given by $\omega RT$ in the framework of $f(R,T)$ gravity and examine the effect of such interaction in spherically symmetric compact stars. Treating the gravity-matter coupling as a perturbative term on the background of Starobinsky gravity, we develop a perturbation theory for equilibrium configurations. For illustration, we take the case of quark stars and explore their various stellar properties. We find that the gravity-matter coupling causes an increase in the stable maximal mass which is relevant for recent observations on binary pulsars.

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Cited by in corpus (2)

• Neutron stars in $f(\mathcal{R},\mathcal{T})$ gravity using realistic equations of state in the light of massive pulsars and GW170817
• Anti-de Sitter neutron stars in the theory of gravity with nonminimal derivative coupling