SU(2) chiral sigma model and properties of neutron stars

We discuss the SU(2) chiral sigma model in the context of nuclear matter us ing a mean field approach at high density. In this model we include a dynam ically generated isoscalar vector field and higher-order terms in the scala r field. With the inclusion of these, we reproduce the empirical values of the nuclear matter saturation density, binding energy, and nuclear incompre ssibility. The value of the incompressibility is chosen according to recent ly obtained heavy-ion collision data. We then apply the same dynamical mode l to neutronrich matter in beta equilibrium, related to neutron star struct ure. The maximum mass and corresponding radius of stable non-rotating neutr on stars are found to be in the observational limit.