论文标题
泰勒不稳定性特征模量的纵向漂移是超慢旋转AP星星的可能解释
Longitudinal drift of Tayler instability eigenmodes as a possible explanation for super-slowly rotating Ap stars
论文作者
论文摘要
从某些AP恒星的磁性变异性推断出的旋转周期非常长，在某些情况下超过十年。缺乏对这种缓慢旋转的解释。本文试图根据AP恒星的磁性和热模式的超慢旋转来解释其内部磁场的不稳定（Tayler）不稳定的不稳定干扰的纵向漂移。使用从A星的结构模型估算的恒星参数计算了Tayler不稳定性的征征局特征模型的漂移和生长速率。计算是指各种强度的环形背景磁场。在共旋转参考框架中，非轴对称不稳定干扰在反旋转方向上漂移。漂移速率随背景场的强度增加。对于超过相等alfven和旋转速度（均衡）值的磁场强度，漂移速率接近恒星的正确旋转速率。在这种情况下，惯性框架中的本征模显示出非常缓慢的旋转。还计算了缓慢旋转的本征模的磁和热干扰模式。 Tayler不稳定性本征模的反旋转漂移是观察到的超高旋转AP恒星现象的可能解释。
Rotation periods inferred from the magnetic variability of some Ap stars are incredibly long, exceeding ten years in some cases. An explanation for such slow rotation is lacking. This paper attempts to provide an explanation of the super-slow rotation of the magnetic and thermal patterns of Ap stars in terms of the longitudinal drift of the unstable disturbances of the kink-type (Tayler) instability of their internal magnetic field. The rates of drift and growth were computed for eigenmodes of Tayler instability using stellar parameters estimated from a structure model of an A star. The computations refer to the toroidal background magnetic field of varied strength. The non-axisymmetric unstable disturbances drift in a counter-rotational direction in the co-rotating reference frame. The drift rate increases with the strength of the background field. For a field strength exceeding the (equipartition) value of equal Alfven and rotational velocities, the drift rate approaches the proper rotation rate of a star. The eigenmodes in an inertial frame show very slow rotation in this case. Patterns of magnetic and thermal disturbances of the slowly rotating eigenmodes are also computed. The counter-rotational drift of Tayler instability eigenmodes is a possible explanation for the observed phenomenon of super-slowly rotating Ap stars.
