Energetics and Propagation of Coronal Mass Ejections in Different Plasma Environments

作     者：Jun LinHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA Jun LinHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA

作者机构：Harvard-Smithsonian Center for Astrophysics 60 Garden Street Cambridge MA 02138 USA 

出 版 物：《Chinese Journal of Astronomy and Astrophysics》 (中国天文和天体物理学报（英文版）)

年 卷 期：2002年第2卷第6期

页      面：539-556页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：This work was supported by NASA grants NAG5-11420 to the Smithsonian Astrophysical Observatory 

主　　题：Sun: CMEs   Sun: atmosphere   Sun: magnetic fields 

摘      要：Based on previous work, we investigate the propagation of CMEs in a more realistic plasma environment than the isothermal atmosphere, and find that it is a slightly faster reconnection for flux ropes to break free. The average Alfven Mach number MA for the inflow into the reconnection site has to be at least 0.013 in order to give a plausible eruption (compared to MA = 0.005 for the isothermal atmosphere). Taking MA = 0.1, we find that the energy output and the electric field induced inside the current sheet match the temporal behavior inferred from the energetic, long duration, CME-associated X-ray events. The results indicate that catastrophic loss of equilibrium in the coronal magnetic field provides the most promising mechanism for major solar eruptions, and that the more energetic the eruption is, the earlier the associated flare peaks. The variation of the output power with the background field strength revealed by our calculations implies the poor correlation between slow CMEs and solar flares. This work also further confirms the explanation we proposed for the peculiar motion of giant X-ray arches and anomalous post-flare loops. Their kinematic pattern and observed heights are determined by the local Alfven speed and its variation with height.