Nuclear equation of state at high density and the properties of neutron stars - art. no. 045801

We discuss the relativistic nuclear equation of state (EOS) using a relativ istic transport model in heavy-ion collisions. From the baryon flow for Au + Au systems at SIS to AGS energies and above we find that the strength of the vector potential has to be reduced moderately at high density or at hig h relative momenta to describe the flow data at (1-10)A GeV. We use the sam e dynamical model to calculate the nuclear EOS and then employ this to calc ulate the gross structure of a neutron star considering the core to be comp osed of neutrons with an admixture of protons, electrons, muons, sigmas, an d lambdas at zero temperature. We then discuss these gross properties of ne utron stars such as maximum mass and radius in contrast to the observationa l values.