| 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 begin{document}$ mathcal{O}(m_s^4) $end{document}![]() ![]() corrections, we examine the structure of compact stars composed of a charged perfect fluid in the context of begin{document}$ f(R,T) $end{document}![]() ![]() gravity. The system of differential equations describing the structure of charged compact stars has been derived and numerically solved for a gravity model with begin{document}$ f(R,T)= R+ 2beta T $end{document}![]() ![]() . For simplicity, we assumed that the charge density is proportional to the energy density, namely, begin{document}$ rho_{rm ch} = alpha rho $end{document}![]() ![]() . 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. |
