Nuclear Equation of State and Neutron Star Structure

Abstract

The hadronic equation of state for a neutron star is discussed with a particular emphasis on the symmetry energy. The results of several microscopic approaches are compared and also a new calculation in terms of the self-consistent Green function method is presented. In addition possible constraints on the symmetry energy coming from empirical information from the neutron skin of finite nuclei are considered.

Comments: Invited talk presented at the Advanced Research Workshop on "Superdense QCD Matter and Compact Stars", Yerevan, Armenia, Sep 27 2003