论文标题
中子星的强场磁性水力学
Strong-field magnetohydrodynamics for neutron stars
论文作者
论文摘要
我们提出了一种磁流失动力学的公式，可用于描述中子恒星内部中强磁场的演变。我们的方法基于将磁性水力动力学视为一种具有单色全局对称性的理论，并为与该对称性相关的流体动力模式开发了有效的田间理论。在可以忽略局部速度和温度变化的机制中，我们得出了在存在强磁场的情况下与电场的对称限制一致的最通用的本构关系。这种本构的关系不仅重现了戈尔德里希（Goldreich）和雷森尼格（Reisenegger）的现象学模型中得出的欧姆衰变，双极扩散和大厅漂移的现象，而且还揭示了磁场的演变中的新术语，这些术语从这种微观模型中很容易看到。该公式可以预测恒定背景磁场周围的小扰动的新扩散行为，以及电场和磁场各个组件之间的两点相关函数。
We present a formulation of magnetohydrodynamics which can be used to describe the evolution of strong magnetic fields in neutron star interiors. Our approach is based on viewing magnetohydrodynamics as a theory with a one-form global symmetry and developing an effective field theory for the hydrodynamic modes associated with this symmetry. In the regime where the local velocity and temperature variations can be neglected, we derive the most general constitutive relation consistent with symmetry constraints for the electric field in the presence of a strong magnetic field. This constitutive relation not only reproduces the phenomena of Ohmic decay, ambipolar diffusion, and Hall drift derived in a phenomenological model by Goldreich and Reisenegger, but also reveals new terms in the evolution of the magnetic field which cannot easily be seen from such microscopic models. This formulation gives predictions for novel diffusion behaviors of small perturbations around a constant background magnetic field, and for the two-point correlation functions among various components of the electric and magnetic fields.
