| In this thesis, we study properties of neutron star in the framework of the relativistic mean field theory of interacting nucleons, hyperons, and mesons. We investigate the influence of different hyperon couplings from analysis of various experimental data on hypernuclei on the composition and equation of state of cold neutron star. We also study neutron star shortly after they are born, when entropy per baryon is 1 or 2 across the star and neutrino may be trapped on dynamical timescales. As the study of properties of warm asymmetric nuclear matte may shed a light on the study of neutron star, the liquid-gas phase transition of warm asymmetric nuclear matte is investigated.In the process of studying the influence of different hyperons couplings on the neutron star, we find that sigma baryons do not appearance is in the neutron star matter, when it experiences a strong repulsive potential. There is the change in maximum mass of the neutron stars with different hyperonic potential, but the change is insignificant.In the study of liquid-gas phase transition of warm asymmetric nuclear matte, we find that, in contrast with one-component system which phase transition depends only on fluctuations of density, the instability which produce a liquid-gas phase separation in asymmetric nuclear matter arise from fluctuations in relative number density of proton. It is in fair agreement with some results obtained by non-relativistic treatments.For the neutron star with finite temperature, we find that the contribution to the pressure by effect of entropy per baryon is relatively smaller than the contribution of hyperons. Thus the compositional variables of equation of state play a more important role than thermal variables for the structure and maximum mass of neutron star.In the investigation of the structure of neutron star shortly after it is born, which neutrino are trapped in the core of the star. We study proto-neutron star consists of only neutron and proton and proto-neutron...
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