| In this thesis, thermal neutron star matters are investigated in the framework of the relativistic mean field theory (RMFT).σ*, ? mesons which can reproduce the strong hyperon-hyperon interactions are incorporated compared with the convention RMFT model. Numerical results show that no matter whether these two mesons are included or not, the influences of temperature on neutron star properties have the same trend. The increase of the temperature suppresses the baryon-nucleon interactions and enhances the hyperonization of neutron star matter. This directly affects the equation of state (EOS) and the maximum mass. As the temperature rises, EOS becomes stiffer in the low and high density regions and softer at the mediate density region. Also, as the increase of the temperature the maximum mass increases. On the other hand, after includingσ* and ? mesons, there are some new results, because the additional attractive interaction for hyperons is introduced. However, effects ofσ* and ? mesons on the main properties of neutron star matter are highly suppressed by the rise of the temperature. In particular, for neutron star matter with the temperature higher than 40MeV, the hyperon-hyperon interactions can be ignored in the RMFT.
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