Neutron star equilibrium configurations within a fully relativistic theory with strong, weak, electromagnetic, and gravitational interactions

Description
We formulate the equations of neutron stars taking into account the strong, weak, electro- magnetic and gravitational interactions within a new fully general relativistic Thomas-Fermi approach. The nuclear interactions are described by the exchange of the sigma, omega, and rho virtual mesons. The constancy of the generalized chemical potential, for short Klein potentials, of the particle species is required as a condition of equilibrium throughout the star. The continuity of the Klein potentials in the transition from the core to the crust imposes the presence of a strong electric field larger than the critical one for vacuum polarization. Correspondingly, the electron density decreases in the core-crust transition region. Such a phenomenon leads to neutron stars with crusts with masses and thickness smaller with respect to the ones of traditional neutron star configurations that satisfy local charge neutrality from the center all the way up to the surface. Estimates of the mass-radius relation are shown.
Organised by F. Burgio