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 nonuniform distributions are studied consistently. The inclusion of hyperons considerably softens the EOS at high densities. The Thomas-Fermi approximation is used to describe the nonuniform matter, which is composed of a lattice of heavy nuclei. The phase transition from uniform matter to nonuniform matter occurs around $0.06 {\mathrm{fm}}^{\ensuremath{-}3},$ and the free neutrons drip out of nuclei at about $2.4\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}4} {\mathrm{fm}}^{\ensuremath{-}3}.$ We apply the resulting EOS to investigate the neutron star properties such as maximum mass and composition of neutron stars.
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