The Effects of Interior Magnetic Fields on the Properties of Neutron Stars in the Relativistic Mean-Field Theory
The Effects of Interior Magnetic Fields on the Properties of Neutron Stars in the Relativistic Mean-Field Theory
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DOI：
10.1086/307921
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发表时间：
1999-11
期刊：
影响因子：
--
通讯作者：
Ye-Fei Yuan;Jian-Nan Zhang
中科院分区：
文献类型：
--
作者：
Ye-Fei Yuan;Jian-Nan Zhang
本文基于核物质的两个非线性σ - ω模型，即，BB和ZM模型，在相对论平均场近似。与线性σ - ω模型和BB模型的结果相反，我们发现在ZM模型中，磁场对核子有效质量m* 的影响并不显著，因此我们预言，如果中子星星内部存在强磁场，则中子星内部的中子可能是超流的.而且，随着磁场B强度的增大，物态方程会变得越来越软。在两个非线性σ - ω模型中，我们讨论了内部磁场对中子星的临界质量、半径、转动惯量、地壳质量、地壳转动惯量和引力红移等总体性质的影响.
We investigate the gross properties of the dense neutron star matter and the structure of the stars under the influence of strong magnetic fields, based on two nonlinear σ - ω models of nuclear matter, i.e., the BB and the ZM models, within the relativistic mean-field approximation. Contrary to the results obtained in the linear σ - ω model and the BB model, we find that the influence of the magnetic field on the effective nucleon mass m* is not significant in the ZM model; therefore, we predict that the neutrons in the interior of a neutron star might be superfluid according to the ZM model, if there is a strong magnetic field in the interior of the star. Moreover, the equations of state (EOSs) will become softer and softer with the increase of the strength of the magnetic field B. We show the effects of the interior magnetic fields on the gross properties of neutron stars, such as the critical masses, their corresponding radii, the moment of inertia, the crust masses, the crust moment of inertia, and the gravitational redshift in both nonlinear σ - ω models.