Charged quark stars in f(R,T) gravity* *JMZP acknowledges financial support from the PCI program of the Brazilian agency "Conselho Nacional de Desenvolvimento Científico e Tecnológico"–CNPq. T. Tangphati was supported by King Mongkut's University of Technology Thonburi's Post-doctoral Fellowship. A. Pradhan thanks IUCCA, Pune, India for providing facilities under associateship programmes

Abstract

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 corrections, we examine the structure of compact stars composed of a charged perfect fluid in the context of gravity. The system of differential equations describing the structure of charged compact stars has been derived and numerically solved for a gravity model with . For simplicity, we assumed that the charge density is proportional to the energy density, namely, . It is demonstrated that the matter-geometry coupling constant β and charge parameter α affect the total gravitational mass and the radius of the star.