磁星的相对论模型：扭曲环面磁场位形
Relativistic models of magnetars: the twisted-torus magnetic field configuration
摘要：
我们发现了磁星平衡磁场组态的广义相对论解，扩展了Colaiuda等人（2008）的先前结果。我们的方法是基于相对论的Grad-Shafranov方程的解决方案，麦克斯韦方程组可以减少在一定的限制。我们得到的平衡解的环形磁场分量被限制在一个有限的区域内的恒星，和极向分量延伸到外部。这些所谓的扭曲环面配置已被发现是在牛顿引力框架下的动力学模拟的最终结果，并且似乎比其他配置更稳定。该解决方案包括高阶多极子，这是耦合到占主导地位的偶极场。我们使用最小能量的参数来约束环向场与极向场的比值。
英文摘要：
We find general relativistic solutions of equilibrium magnetic field configurations in magnetars, extending previous results of Colaiuda et al. (2008). Our method is based on the solution of the relativistic Grad-Shafranov equation, to which Maxwell's equations can be reduced in some limit. We obtain equilibrium solutions with the toroidal magnetic field component confined into a finite region inside the star, and the poloidal component extending to the exterior. These so-called twisted-torus configurations have been found to be the final outcome of dynamical simulations in the framework of Newtonian gravity, and appear to be more stable than other configurations. The solutions include higher order multipoles, which are coupled to the dominant dipolar field. We use arguments of minimal energy to constrain the ratio of the toroidal to the poloidal field.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
