Neutron Star Structure In A Nonlinear Realization Of Chiral SU(3) Spontaneous Breaking Model

Since hadrons are excitations with respect to vaccum, hadronic properties have very important relation with the properties of vaccum. At finite baryon densities, the underlying theory of strong interaction, QCD, is not solvable in the nonperturbative low-energy regime. Chiral symmetry spontaneous breaking and confinement are two very important properties of low energy QCD. According to Goldstone theorem, the Goldstone bosons with zero mass will emerge as the chiral symmetry is spontaneously broken. In this paper, we take a way which realizes this constraint by a nonlinear method and generalize the chiral effictive model to SU(3) including the baryon octet. By this means, we obtain the chiral symmetry spontaneous breaking Lagrange density which depicts the strong interactions.It is widely known that the relativistic mean field (RMF) method is rather successful in the researches of nuclear matter, finite nuclei and other fields. In our paper, we use the basical spirit of RMF in practical calculation.By applying RMF approximation into our newly-developed Lagrange density, we study some basic properties of neutron star. The results show that - condensate appears at some baryon densities and makes great effect to the curve of state equation of neutron star; hyperons - and A exist in neutron star matter at high desities. In this model, neutron star's maximum mass is 1.12Ms, with corresponding radius about 8Km.