AI 中文总结
研究固体中磁旋转不稳定性的条件，发现只有当剪切流足够强时，弹性抑制效应才会被克服，并应用于中子星合并前的磁场放大。
AI 中文摘要
磁旋转不稳定性可以在磁化剪切流中产生强烈的湍流子结构。该机制作为流体微观物理方面（如分层和扩散率）的函数已被广泛探索。然而，迄今为止尚未研究的一个方面是这种不稳定性是否也能在固体中运行。受行星或简并星内部固态区域在其生命周期的某个阶段可能相对于液态或气态层存在差分旋转的启发，我们研究了弹性对不稳定性的抑制程度。一个简化的平行平面分析表明，只有当流动发生强烈剪切，使得液体中由不稳定性产生的磁张力超过弹性腔的剪切模量时，才能发生磁增长。在双中子星合并的动力潮汐背景下，这意味着只有在恒星自转频率$\gtrsim 300$Hz时，才能在合并前在壳层中放大磁场。如果粘性加热在共振前削弱了晶体结构，所需的自转频率会降低。
英文摘要
The magnetorotational instability can generate strong, turbulent substructure within magnetized shear flows. The efficacy of the mechanism as a function of microphysical aspects of the fluid, such as stratification and diffusivity, has been explored extensively. One aspect that has not been studied thus far, however, is whether the instability can also operate in solids. Motivated by the possibility that solid regions within planets or degenerate stars may rotate differentially with respect to liquid or gaseous layers during some phase of their life, we examine the extent to which elasticity suppresses the instability. A simplified, plane-parallel analysis reveals that only in cases where the flow is strongly sheared, such that the magnetic tension that would result from the instability in a liquid exceeds the shear modulus of the elastic cavity, can magnetic growth occur. In the context of dynamical tides in binary neutron-star mergers, this implies that the magnetic field can be amplified in the crust prior to coalescence only if the star boasts a spin frequency of $\gtrsim 300$Hz. If viscous heating weakens the crystalline structure prior to resonance, the required spin frequency is reduced.
Comments13 pages, 4 figures. Minor changes to match PRD style
