| Energetics and Propagation of Coronal Mass Ejections in Different Plasma Environments |
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| 作者姓名： | Jun LinHarvard-Smithsonian Center for Astrophysics Garden Street Cambridge MA USA |
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| 作者单位： | Jun LinHarvard-Smithsonian Center for Astrophysics，60 Garden Street，Cambridge，MA 02138，USA |
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| 基金项目： | This work was supported by NASA grants NAG5-11420 to the Smithsonian Astrophysical Observatory. |
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| 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. Th
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Energetics and Propagation of Coronal Mass Ejections in Different Plasma Environments |
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| Jun LinHarvard-Smithsonian Center for Astrophysics, Garden Street,Cambridge,MA ,USA.Energetics and Propagation of Coronal Mass Ejections in Different Plasma Environments[J].Chinese Journal of Astronomy and Astrophysics,2002,2(6). |
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| Authors: | Jun Lin |
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| Institution: | Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA |
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| Abstract: | Based on previous work, we investigate the propagation of CMEs in amore realistic plasma environment than the isothermal atmosphere, and find thatMach number MA for the inflow into the reconnection site has to be at least 0.013in order to give a plausible eruption (compared to MA = 0.005 for the isothermalatmosphere). Taking MA = 0.1, we find that the energy output and the electricfield induced inside the current sheet match the temporal behavior inferred fromthe energetic, long duration, CME-associated X-ray events. The results indicatethat catastrophic loss of equilibrium in the coronal magnetic field provides the mostpromising mechanism for major solar eruptions, and that the more energetic theeruption is, the earlier the associated flare peaks. The variation of the output powerwith the background field strength revealed by our calculations implies the poor cor-relation between slow CMEs and solar flares. This work also further confirms theexplanation we proposed for the peculiar motion of giant X-ray arches and anoma-lous post-flare loops. Their kinematic pattern and observed heights are determined by the local Alfven speed and its variation with height. |
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| Keywords: | Sun: CMEs - Sun: atmosphere - Sun: magnetic fields |
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