Abstract
A relativistic field theory of isospin asymmetric matter and of neutron star matter in particular, which is compatible with nuclear matter bulk properties, was formulated in Part I of this series and treated in mean-field approximation. The self-consistent solutions include the σ, ω, and ϱ-fields for both the normal and pion-condensed states. The bulk properties of nuclear matter such as saturation density and energy, compressibility and asymmetry energy impose rather stringent restrictions on meson-nucleon coupling constants and the parameters of the nonlinear interactions in the σ-model. The numerical results include the equation of state, particle densities as functions of charge and baryon density and the composition of a neutron star. Based on these results, we discuss neutron star cooling for various equations of state.
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