The review begins with an introduction to some of the various solar phenomena that may be investigated using stability theory. The geometry of the coronal magnetic field for many models is either a loop or an arcade and it is the stability properties of these structures that are investigated. The author presents a simple physical description of the basic MHD instabilities and describes the main difference between laboratory and coronal plasmas due to the presence of an extremely dense plasma at the footpoints of the coronal magnetic fieldlines. The implications of this density interface are discussed. Linear stability theory is applied to some solar situations and some non-linear simulations are discussed.
本综述首先介绍了一些可以利用稳定性理论研究的各种太阳现象。许多模型中日冕磁场的几何结构要么是环状，要么是拱状，而研究的正是这些结构的稳定性性质。作者对基本的磁流体动力学不稳定性给出了简单的物理解释，并描述了实验室等离子体与日冕等离子体之间的主要区别，这种区别源于日冕磁力线足点处存在极其致密的等离子体。讨论了这一密度界面的影响。将线性稳定性理论应用于一些太阳实际情境，并讨论了一些非线性模拟结果。