中子星中简并电子气体的临界磁化  

Critical magnetization of degenerate electronic system in neutron star

作　　者：王兆军 吕国梁[2] 朱春花[2] 张军[1,2] 

机构地区：[1]西安交通大学理学院应用物理系,西安710049 [2]新疆大学物理学院,乌鲁木齐830046

出　　处：《物理学报》2011年第4期829-835,共7页Acta Physica Sinica

基　　金：国家自然科学基金(批准号:10963003)资助的课题~~

摘　　要：中子星内部的电子处于高度简并或完全简并的状态,电子磁矩(包括内禀磁矩和朗道反磁矩)的取向不是随机的,而是呈现出极强的磁化行为.考虑了磁化后的磁诱导方程要改写,改写后的方程添加了新的磁场生成项,更重要的改变是等效磁扩散系数变小了(顺磁情况),在临界情况(等效扩散系数等于零),磁场在磁生成项的作用下增加直到抑制机理出现,朗道反磁矩就是在这个时候变得越来越重要.磁场增加的最终结果使中子星局域磁场成为振荡的,对外看来有可能成为磁星.Degenerate electronic Fermi system with intrinsic（spin） magnetic moment and Landau diamagnetic moment of the electrons in a neutron star interior is magnetized.Taking the magnetizing effect into consideration,the magnetic induced equation must be changed：the resulting equation has an additional magnetic induction term and a magnetic diffusion coefficient that is different from the original one for plasma.When effective magnetic diffusion coefficient equals critical value（zero） the fully degenerate electronic system approaches a new phase.In this phase,the magnetic field of neutron star will become very large until other mechanisms suppress the increasing of the field in the neutron star lowered crust.For a stable or de Hass-Van Alphen oscillatory state,it is possible for the neutron star to become a magnetar.

关 键 词：中子星 简并 磁化 

分 类 号：P145.6[天文地球—天体物理]