MASS, RADIUS AND MOMENT OF INERTIA OF NEUTRON STARS
Abstract
We construct the ground-state equilibrium configurations of neutron star cores. The system of equilibrium equations, taking into account quantum statistics, electro-weak, and strong interactions, is formulated within the framework of general relativity both in the rotating and 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 mediated by the sigma-omega-rho virtual mesons. The mass-radius relation for neutron star cores is obtained for various parametrizations of the nuclear model. The equilibrium conditions are given by our recently developed theoretical framework based on the Einstein-Maxwell-Thomas-Fermi equations along with the constancy of the general relativistic Fermi energies of particles, the "Klein potentials", throughout the configuration. These equations are here solved numerically in the case of zero temperatures and for selected parameterizations of the nuclear model. We present here the new neutron star mass-radius relation.
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