Complete relativistic equation of state for neutron stars
H. Shen
Abstract
We construct the equation of state (EOS) in a wide density range for neutron stars using the relativistic mean field theory. The properties of neutron star matter with both uniform and non-uniform distributions are studied consistently. The inclusion of hyperons considerably softens the EOS at high densities. The Thomas-Fermi approximation is used to describe the non-uniform matter, which is composed of a lattice of heavy nuclei. The phase transition from uniform matter to non-uniform matter occurs around 0.06 fm-3, and the free neutrons drip out of nuclei at about 2.4 × 10-4\ fm-3. We apply the resulting EOS to investigate the neutron star properties such as maximum mass and composition of neutron stars.
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