论文标题
非轴对称霍尔不稳定性：了解磁铁的关键
Nonaxisymmetric Hall instability: A key to understanding magnetars
论文作者
论文摘要
人们普遍认为，中子星体内部磁场的非线性动力学演化在解释观察到的现象学的解释中起着关键作用。了解环形和多型组件之间或不同尺度之间的能量传递特别相关。在这封信中，我们介绍了中子恒星外壳中霍尔不稳定性的第一个3D模拟，证实了其在典型的磁性条件下的存在。我们面对通过线性扰动分析获得的估计结果，该分析将任何解释视为数值不稳定性并确认其物理起源。有趣的是，霍尔不稳定性会产生局部强的磁性结构，偶尔会使地壳产量到磁应力并产生冠状环，就像太阳能冠状动脉环通过光电孔找到了出路。这支持了该机制的生存能力，该机制已提出解释磁性爆发。
It is generally accepted that the non-linear, dynamical evolution of magnetic fields in the interior of neutron stars plays a key role in the explanation of the observed phenomenology. Understanding the transfer of energy between toroidal and poloidal components, or between different scales, is of particular relevance. In this letter, we present the first 3D simulations of the Hall instability in a neutron star crust, confirming its existence for typical magnetar conditions. We confront our results to estimates obtained by a linear perturbation analysis, which discards any interpretation as numerical instabilities and confirms its physical origin. Interestingly, the Hall instability creates locally strong magnetic structures that occasionally can make the crust yield to the magnetic stresses and generates coronal loops, similarly as solar coronal loops find their way out through the photosphere. This supports the viability of the mechanism, which has been proposed to explain magnetar outbursts.
