Numerical and Theoretical Studies of Solar Magnetic Field Structure, Coronal Heating and Solar Convection

这项工作旨在阐明日冕环在光球层对流引起的足点运动所施加的应力下的磁性微结构。微结构决定了(I)先前假设的单个电流层的范围和宽度，(Ii)沿场线的电流的丝状化和由此产生的增强的耗散。这也可能导致随机磁场的存在，使剪切Alfven波的速度大大增强。因此，磁性微结构在促成太阳日冕加热的物理过程中起着关键作用。这种微结构在重新连接过程中也是关键的，重新连接过程将应力磁场松弛到较低的能量状态。这些过程是使用一个数学模型来研究的，该模型通过解析和数值模拟来处理。计算结果与观测数据进行了比较。***

This work is directed to the elucidation of the magnetic microstructure of coronal loops under the stresses imposed by footpoint motion due to photospheric convection. The microstructure determines the (i) the extent and width of the singular current layers postulated earlier, (ii) the filamentation of the current flow along the field lines and the resultant enhanced dissipation. It could also lead to the presence of stochastic magnetic fields with a greatly enhanced rate for shear Alfven waves. Thus the magnetic microstructure plays a critical role in the physical processes that contribute to solar coronal heating. This microstructure is also critical in the reconnection processes which relax the stressed magnetic field to a lower energy state. These processes are investigated using a mathematical model that is treated both analytically and through numerical simulation. The calculations thus obtained are compared with observational data. ***