The Crust Of Neutron Star And Symmetry Energy

This paper discussed the neutron stars in detail about their formation process, observationmechanisms, conformation, development course and significance, and reviewed the researchhistory of neutron stars and the findings obtained by those studies home and abroad. On the baseof these findings, this paper mainly carried out two researches.In the first part, on the base of quantum field theory of relativity many-body system, we usedthe mean field approximation of relativity meson model to discuss the relationsbetween nuclear symmetry energy of the crust nuclear matter of neutron star andincompressibilities. Findings showed that as the baryon density increased, the symmetry energygrew at different coupling constants. Furthermore, the symmetry energy at saturation densityincreases with increasing incompressibility at fixed d, and decreases at fixed c. Specifically,when coupling constantsg vandg swere fixed, respectively, the symmetry energy changed alittle with increasing incompressibility. It demonstrates that compared to self-coupling constants,N-N coupling constants were more influential on the symmetry energy.In the second part, we abandoned the empirical formula, introduced the boundary condition ofthe meson to explore the inhomogeneous meson field equation and used Thomas-Fermiapproximation to describe the equation of state (EOS) of the neutron star crust matter. Findingsshowed that the average energy density and the pressure of the matter increased with theincreasing density of nucleon, the number of densities and the energy density of nucleonsdecreased from the center in the cell. The radius decreased whenn Bincreases and the nucleidissolved whennB0.06fm3. These results are fairly consistent with existing findings, whichmeans the production of self-consistent model is successful.