Inner Crust of Neutron Stars in Relativistic Mean Field Approach  

作　　者：CAO Ji-guang MA Zhong-yu Nguyen Van Gia 

机构地区：[1]Institute of Nuclear Physics, Paris University, France [2]不详

出　　处：《Annual Report of China Institute of Atomic Energy》2007年第1期83-84,共2页中国原子能科学研究院年报（英文版）

基　　金：National Natural Science Foundation of China (10475116, 10535010);Major State Basic Research Development Program in China (2007CB815000);European Community Project Asia-Europe Link in Nuclear Physics and Astrophysics, CN/ASIA-LINK/008(94791)

摘　　要：The microscopic properties and superfluidity of the inner crust in neutron stars are investigated in the framework of the relativistic mean field (RMF) model. The Wigner-Seitz (W-S) cell of inner crustThe microscopic properties and superfluidity of the inner crust in neutron stars are investigated in the framework of the relativistic mean field （RMF） model. The Wigner-Seitz （W-S） cell of inner crust is composed of neutron-rich nuclei immersed in a sea of dilute, homogeneous neutron gas. In this work, we emphasize on the choice of the boundary conditions in the RMF approach. Three kinds of boundary conditions are suggested. The properties of the W-S cells with the three kinds of boundary conditions are investigated.

关 键 词：核物理学 中子星 内壳 相对平均场法 

分 类 号：P145.6[天文地球—天体物理]