HYDROMAGNETIC INSTABILITIES IN RELATIVISTIC NEUTRON STARS
HYDROMAGNETIC INSTABILITIES IN RELATIVISTIC NEUTRON STARS
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DOI：
10.1088/2041-8205/735/1/l20
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发表时间：
2011-05
期刊：
影响因子：
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通讯作者：
P. Lasky;B. Zink;K. Kokkotas;K. Glampedakis
中科院分区：
文献类型：
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作者：
P. Lasky;B. Zink;K. Kokkotas;K. Glampedakis
在广义相对论中，假设中子星的状态方程为多变的，建立了极向磁场的非线性理想磁流体动力学模型。我们识别了常见的流体磁模，特别是极向磁场固有的“香肠/曲张”模式和“扭结”不稳定性。这种演化是由扭结不稳定性主导的，扭结不稳定性导致了磁场的剧变重构。系统随后演化为新的非轴对称准平衡端态。稳定准平衡的这一分支的存在可能会对磁物理学产生影响，包括耀斑的产生机制和对准周期振荡的解释。
We model the nonlinear ideal magnetohydrodynamics of poloidal magnetic fields in neutron stars in general relativity assuming a polytropic equation of state. We identify familiar hydromagnetic modes, in particular the “sausage/varicose” mode and “kink” instability inherent to poloidal magnetic fields. The evolution is dominated by the kink instability, which causes a cataclysmic reconfiguration of the magnetic field. The system subsequently evolves to new, non-axisymmetric, quasi-equilibrium end states. The existence of this branch of stable quasi-equilibria may have consequences for magnetar physics, including flare generation mechanisms and interpretations of quasi-periodic oscillations.