Boundary Conditions of Wigner-Seitz Cell in Inner Crust of Neutron Stars with Relativistic Mean Field Approach
Boundary Conditions of Wigner-Seitz Cell in Inner Crust of Neutron Stars with Relativistic Mean Field Approach
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DOI：
10.1088/0256-307x/25/1/021
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发表时间：
2008
影响因子：
3.5
通讯作者：
Cao Ji-guang;Yang Ding;Ma Zhong-yu;N. Giai
中科院分区：
文献类型：
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作者：
Cao Ji-guang;Yang Ding;Ma Zhong-yu;N. Giai
用相对论平均场方法研究了中子星内壳维格纳-塞茨(W-S)盒的微观结构。W-S池由位于中心周围区域的一团中子和质子组成，周围环绕着密度大致均匀的中子气。为了产生W-S胞体的密度，在单粒子波函数的计算中需要适当的边界条件。重点讨论了RMF方法中边界条件的选择。提出了三种边界条件。研究了三种边界条件下W-S池的性质。比较了RMF模型和Hartree-Fock-Bogoliubov(HFB)模型中的中子密度分布。结果表明，在RMF模型中，W-S池的中子气密度高于在HFB模型中得到的中子气密度。
The microscopic structure of the Wigner–Seitz (W-S) cell in the inner crust of neutron stars is investigated with the relativistic mean field (RMF) approach. The W-S cell is composed of a cluster of neutrons and protons localized in a region around the centre and surrounded by a neutron gas of approximately uniform density. In order to generate the density of the W-S cell, appropriate boundary conditions in the calculation of the single-particle wavefunctions are necessary. 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 cell with the three kinds of boundary conditions are investigated. The neutron density distributions in the RMF and Hartree–Fock–Bogoliubov (HFB) models are compared. It is found that the neutron gas densities of the W-S cell in the RMF model is higher than those obtained in the HFB model.