Symmetry Energy and Neutron Star Equation of State

Abstract

Information about many aspects of both nuclear physics and a neutron star structure are encoded in the density dependence of the symmetry energy. Despite the fact that considerable progress has been made in constraining the density dependence of the symmetry energy, it is still the most uncertain part of the asymmetric nuclear matter equation of state (EOS). The analysis of neutron star parameters which are most sensitive to the form of the symmetry energy in the case of nucleon and strangeness-rich matter has been done with the use of the relativistic mean field (RMF) approximation. The mixed vector meson interactions have been introduced to modify the density dependence of the symmetry energy.