Shear Flow Instabilities in Rotating Shallow-Water MHD

太阳物理学中最令人兴奋的观测发现之一是在对流层底部的塔可跃层，这是一个具有高速剪切和强磁场的薄区域。该项目将考虑该区域可能存在的不稳定性，并考虑旋转的影响；将使用浅水MHD方程来适应塔乔跃层的小深度。该项目将从理想化流动和磁场的线性不稳定性开始，这将进行分析研究，然后转移到更一般的流动和场分布，这将需要数值方法。然后，该项目将继续考虑这些不稳定性的非线性演化，以及它们与太阳内部交通的相关性。

One of the most exciting observational discoveries in solar physics was that of the tachocline, a thin region of high velocity shear, and strong magnetic field, at the base of the convection zone. This project will consider the possible instabilities of this region, incorporating the influence of rotation; the small depth of the tachocline will be accommodated by using the shallow water MHD equations. The project will start with the linear instability of idealised flows and magnetic fields, which will be studied analytically, before moving on to more general flow and field profiles, which will require a numerical approach. The project will then move on to consider the nonlinear evolution of these instabilities, andtheir relevance to transport in the solar interior.