The Study Of The Property Of Neutron Star Matter

In this paper, firstly introduce the structure and properties of neutron stars, then overview the history of research on neutron stars and point out variety of research mod-els and their characteristics. To the research of neutron star the most important input is the equation of state (EOS). Different equation of state would lead to different re-sults of numerical simulation. At present, the main theory is based on relativistic mean field (RMF) theory, considering different interaction models, extending from the already known knowledge of nuclear physics to high-density, high magnetic field of neutron star matters.Our research is numerical solving the equation of state and relativistic equation (TOV) which describe the structure of a static star with spherical symmetry. Get two series of results, the difference is whether the component of the star include hyperon. In both cases, we get the maximum mass and relative radius. Comparing the numerical results to observable results, we found out that most of the neutron stars contain hyperon.Based on the relativisticσ—ω—ρmodel, considering the interaction betweenσ,ω,ρmeson and nucleons, presuming the components are only neutron, proton and electron, I studied the equation of state of neutron stars' matter. We found out that under a constant temperature, the pressure increases when energy density increases, and the higher the temperature the stiffer the EOS. At the mean time, we also found out that when the temperature is constant, the percentage of neutron raise and the percentage of proton lower when the particle number density raise. When the star is hotter, the percentage of neutron decrease a little and the percentage of proton increase a little.