Neutron stars within a general relativistic theory including strong, weak and electromagnetic interactions

We construct the ground-state equilibrium configurations of neutron stars. The system of equilibrium equations is obtained taking into account quantum statistics, electro-weak, and strong interactions, within the framework of general relativity in the non-rotating spherically symmetric case. The core is assumed to be composed of interacting degenerate neutrons, protons and electrons in beta equilibrium. The strong interaction between nucleons is modeled through sigma-omega-rho meson exchange model. The mass-radius relation for neutron star cores is obtained for the various nuclear parametrizations. The mass and the thickness of the outer crusts corresponding to the different core mass-radius relations are obtained. The analysis is performed for two selected equations of state (EoS)of the outer crust matter. The first one neglects the Coulomb interactions between the degenerate electrons and the nuclear component of fixed charge to mass ratio Z/A. The second EoS, takes into account the Coulomb interactions of the point-like nuclei with a uniform fluid of degenerate electrons and the nuclear contribution is obtained from experimental data of nuclear masses. The mass and the thickness of the outer crust obtained with these two different EoS are compared and contrasted. We obtain systematically outer crusts with smaller mass and larger thickness when Coulomb interactions are taken into account.