On hydrodynamic stability of weakly magnetized stellar radiative zones
On hydrodynamic stability of weakly magnetized stellar radiative zones
复制标题
弱磁化恒星辐射区的流体动力学稳定性
DOI：
10.1093/mnras/280.1.149
复制
发表时间：
1996
影响因子：
4.8
通讯作者：
V. Urpin
中科院分区：
文献类型：
--
作者：
V. Urpin
我们考虑弱磁化差分旋转恒星对绝热轴对称扰动的稳定性。分析了角速度取决于球面半径和极角的一般情况。在磁化辐射区中，存在两种低频模式，即浮力阿尔文模式和扭转阿尔文模式，它们可以通过差速旋转而变得不稳定。对于不稳定，浮力模式需要从两极到赤道方向的比角动量减小，而如果角速度从两极到赤道减小，则阿尔文模式可能不稳定。相对较强的磁场可以稳定这两种模式。
We consider the stability of weakly magnetized differentially rotating stars to adiabatic axisymmetric disturbances. The general case of the angular velocity being dependent on both the spherical radius and the polar angle is analysed. In magnetized radiative zones, there are two low-frequency modes, the buoyant and torsion Alfven ones, which can be destabilized by a differential rotation. For instability, the buoyant mode requires a decrease of the specific angular momentum in the direction from the poles to the equator, whereas the Alfven mode can be unstable if the angular velocity decreases from the poles to the equator. A relatively strong magnetic field may stabilize both of these modes.