Relativistic stars with purely toroidal magnetic fields
Relativistic stars with purely toroidal magnetic fields
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DOI：
10.1103/physrevd.78.044045
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发表时间：
2008-02
影响因子：
5
通讯作者：
K. Kiuchi;Shijun Yoshida
中科院分区：
文献类型：
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作者：
K. Kiuchi;Shijun Yoshida
我们研究了纯环面磁场对相对论性恒星平衡结构的影响。首次导出了含纯环面磁场的相对论性旋转恒星平衡解的基本方程。为了在数值上求解这些基本方程，我们扩展了Cook-Shapiro-Teukolsky格式来计算不含磁场的相对论性旋转恒星，以纳入纯环面磁场的影响。通过数值格式，我们计算了特定磁场分布下的大量平衡构型，以探索平衡性质。我们还构建了恒定重子质量和/或恒定磁通量的平衡序列，这些序列模拟了孤立中子星通过引力波失去角动量时的演化。本研究得到的磁化恒星平衡构型的重要性质总结如下：(1)对于非旋转恒星，由于环向磁场的作用，恒星的物质分布会长期扭曲。(2)对于快速旋转的恒星，由于离心力的作用，恒星表面的形状变得扁平化。但是，恒星内部深处的物质分布足以使恒星的平均物质分布延长。(3)较强的环面磁场导致恒星在较低角速度下的质量脱落。(4)对于某些重子质量和磁通量恒定的平衡序列，恒星在失去角动量时可以自旋向上。
We investigate the effects of the purely toroidal magnetic field on the equilibrium structures of the relativistic stars. The basic equations for obtaining equilibrium solutions of relativistic rotating stars containing purely toroidal magnetic fields are derived for the first time. To solve these basic equations numerically, we extend the Cook-Shapiro-Teukolsky scheme for calculating relativistic rotating stars containing no magnetic field to incorporate the effects of the purely toroidal magnetic fields. By using the numerical scheme, we then calculate a large number of the equilibrium configurations for a particular distribution of the magnetic field in order to explore the equilibrium properties. We also construct the equilibrium sequences of the constant baryon mass and/or the constant magnetic flux, which model the evolution of an isolated neutron star as it loses angular momentum via the gravitational waves. Important properties of the equilibrium configurations of the magnetized stars obtained in this study are summarized as follows: (1) For the nonrotating stars, the matter distribution of the stars is prolately distorted due to the toroidal magnetic fields. (2) For the rapidly rotating stars, the shape of the stellar surface becomes oblate because of the centrifugal force. But, the matter distribution deep inside the star is sufficiently prolate for the mean matter distribution of the star to be prolate. (3) The stronger toroidal magnetic fields lead to the mass shedding of the stars at the lower angular velocity. (4) For some equilibrium sequences of the constant baryon mass and magnetic flux, the stars can spin up as they lose angular momentum.