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

这项工作是针对阐明的磁性 冠环的显微结构下施加的应力， 由于光球对流而引起的足点运动。的 微结构决定（i）微结构的范围和宽度， 奇异电流层假设较早，（ii） 电流沿着场线的方向和磁场的方向 从而增强耗散。这也可能导致 随机磁场的存在大大增强了 剪切阿尔芬波的速率。因此，磁性微结构 在物理过程中起着关键作用， 太阳日冕加热。这种微结构也是关键， 重联过程使受应力的磁 场到较低的能量状态。研究了这些过程 使用一个数学模型，该模型被分析地处理， 通过数值模拟。 由此获得的计算结果为： 与观测数据相比。***

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. ***