Neutron Star Structure in a Nonlinear Realization of Chiral SU（3）.Spontaneous Breaking Model  

作　　者：CHENHan LüXiao-Fu 

机构地区：[1]DepartmentofPhysics,SichuanUniversity,Chengdu610064,China [2]CCAST（WorldLaboratory）,P.O.Box8730,Beijing100080,ChinaInstituteofTheoreticalPhysics,AcademiaSinica,P.O.Box2735,Beijing100080,China

出　　处：《Communications in Theoretical Physics》2004年第3期447-453,共7页理论物理通讯（英文版）

基　　金：The project supported in part by the Key Research Plan of Theoretical Physics and Cross Science under Grant No.90103018;;National Natural Science Foundation of China under Grant No.19975062

摘　　要：We investigate neutron star properties by constructing a chiral SU(3) spontaneous breaking Lagrangian and using relativistic mean-field approximation. The results show that condensate appears at some baryon densities, and hyperons and exist in neutron star matter at high density. In this model, neutron star's maximum mass is with corresponding radius about 8 km.

关 键 词：chiral SU(3) spontaneous breaking beta stable Oppenheimer-Volkoff equations 

分 类 号：P145.6[天文地球—天体物理]