日冕物质抛射的两个能量释放过程：MHD突变和磁重联
Two Energy Release Processes for CMEs: MHD Catastrophe and Magnetic Reconnection
摘要：
日冕中的磁能是如何快速释放的，从而产生太阳耀斑和日冕物质抛射（CME）等太阳爆炸，这仍然是一个悬而未决的问题。最近的研究已经证实，一个系统的磁通绳嵌入在一个背景场表现出灾难性的行为，在灾难点的能量阈值可能会超过相关的开放领域的能量。日冕中积累的自由能在灾变发生时突然释放，至少在初始阶段可能是日冕物质抛射能量释放的主要方式。与磁重联等非理想过程相比，这种释放是通过理想的MHD过程进行的。这一突变导致了电流片的突然形成，这自然为快速磁重联提供了合适的位置。这种重连一方面可以被确认为与CME有关的太阳耀斑，另一方面又进一步加速了CME。在此基础上，对今后的观测研究，特别是利用"夸父“卫星，研究MHD灾变和磁重联在与日冕物质抛射和耀斑有关的磁能释放中的作用，提出了几点初步建议。
英文摘要：
It remains an open question how magnetic energy is rapidly released in the solar corona so as to create solar explosions such as solar flares and coronal mass ejections (CMEs). Recent studies have confirmed that a system consisting of a flux rope embedded in a background field exhibits a catastrophic behavior, and the energy threshold at the catastrophic point may exceed the associated open field energy. The accumulated free energy in the corona is abruptly released when the catastrophe takes place, and it probably serves as the main means of energy release for CMEs at least in the initial phase. Such a release proceeds via an ideal MHD process in contrast with nonideal ones such as magnetic reconnection. The catastrophe results in a sudden formation of electric current sheets, which naturally provide proper sites for fast magnetic reconnection. The reconnection may be identified with a solar flare associated with the CME on one hand, and produces a further acceleration of the CME on the other. On this basis, several preliminary suggestions are made for future observational investigations, especially with the proposed KuaFu satellites, on the roles of the MHD catastrophe and magnetic reconnection in the magnetic energy release associated with CMEs and flares.
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