Physics – Nuclear Physics – Nuclear Theory
Scientific paper
2002-02-09
Phys.Rev. C65 (2002) 035802
Physics
Nuclear Physics
Nuclear Theory
23 pages, REVTeX, 9 ps figures, to appear in Phys. Rev. C
Scientific paper
10.1103/PhysRevC.65.035802
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 $0.06 \rm{fm^{-3}}$, and the free neutrons drip out of nuclei at about $2.4 \times 10^{-4}\ \rm{fm^{-3}}$. We apply the resulting EOS to investigate the neutron star properties such as maximum mass and composition of neutron stars.
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