Charged quark stars in f(R,T) gravity

Recent advances in nuclear theory and new astrophysical observations have led to the need for specific theoretical models applicable to dense-matter physics phenomena. Quantum chromodynamics (QCD) predicts the existence of non-nucleonic degrees of freedom at high densities in neutron-star matter, such as quark matter. Within a confining quark matter model, which consists of homogeneous, neutral 3-flavor interacting quark matter with O(m(s)(4)) corrections, we examine the structure of compact stars composed of a charged perfect fluid in the context of f (R,T) gravity. The system of differential equations describing the structure of charged compact stars has been derived and numerically solved for a gravity model with f(R, T) = R + 2 beta T. For simplicity, we assumed that the charge density is proportional to the energy density, namely, rho(ch) = alpha rho. It is demonstrated that the matter-geometry coupling constant beta and charge parameter alpha affect the total gravitational mass and the radius of the star.