在太阳爆发过程中，一般在耀斑和CME之间会有一个长的电流片形成。其中发生磁重联对爆发来说是一个关键的过程，它将磁能迅速转化为等离子体的动能和热能，并加速高能粒子。由于长的电流片对各种等离子体的湍流不稳定，因此其中会产生多种尺度的磁场/等离子结构，这些结构的发展和演化在很大程度上影响磁重联过程。也就是说，磁重联是一个发生在多个尺度的过程，是各个尺度上发生过程的耦合。借助MHD数值实验，以太阳爆发磁通量绳灾变模型为基础，我们可以为磁重联电流片不同尺度的演化提供理论参考，从而帮助我们理解电流片的内部结构与磁重联速率的内在联系。同时，改进MHD数值算法，加入研究适用于太阳爆发的边界条件，优化并行程序及改造程序相匹配的仪器搭配也是本项目的目标之一。

In the process of solar eruptions, it generally forms a long and thin current sheet (CS) between flares and CMEs, wherein magnetic reconnection plays a key role in energy conservation. It converts magnetic energy into plasma kinetic and thermal energy, even allows for particle acceleration. A long CS can yield multi-scale magnetic fields or various plasmoids due to turbulence instability, which affects largely the reconnection rate. In other words, magnetic reconnection is a consequence of multi-scale coupling states. Using MHD simulations, we can make a numerical study of flux rope model for solar eruption, analyzing the CS evolution in multi-scales during magnetic reconnection process, in order to better understand the lively mechanism related to internal structures of CS and reconnection rate. Meanwhile, to improve the MHD algorithm, by setting suitable boundary conditions for solar environment, updating the MPI codes and customizing the computing platforms, is also a main goal in this work.