The Study Of The Equation Of State Of Neutron Star Matter

In this paper, we discussed the neutron stars in detail about their conformation and properties. We reviewed the research history of neutron stars, the results which have been obtained by the studies of the equations of state (EOS) of neutron star matters all over the world. Then, with the quantum field theory of relativity many-body system, we used the mean field approximation of relativity a -ωmodel to deduce the EOS of homogeneous and static nuclear matters. According to the saturation property of infi-nite homogeneous nuclear matters, using numerical simulation we obtained the coupling constants between nucleus and meson and the self-coupling constants among sigma me-son. Influence of the self-coupling constants on im-compressibility coefficient is great important.Using the model and parameters which we have mentioned before, we studied the EOS of nuclear matters which there are only proton, neutron and electron, and the vari-ation of composition with the baryon number density. Noticing that, inside the neutron stars, the energy and pressure density are increased and increased faster and faster when the baryon density is increased; meanwhile, the fraction of neutron is decreased and the proton's is increased.In the last part of this paper, using the Thomas-Fermi approximation, we studied the effect of spin to the energy density, neutron density and scalar density inside a cell at the outer crust of neutron star and compared the difference among spherically symmetric cell and cylindrically symmetric cell. We found that when the neutron star rotating with a period is 0.5ms the effect is enormous to the energy density and neutron density and is little to the scalar density, and all the results in the spherically symmetric cell is bigger than which in the cylindrically symmetric cell in the same conditions.