Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmng31a1184c&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #NG31A-1184
Physics
7513 Coronal Mass Ejections (2101), 7519 Flares, 7526 Magnetic Reconnection (2723, 7835)
Scientific paper
Impulsive magnetic reconnection has been considered as the mechanism responsible for impulsive non- thermal emission in hard X-rays (HXR) and millimeter/submillimeter waves during the soft X-ray (SXR) flare rise phase. The impulsive non-thermal emission also correlates temporarily with impulsive acceleration of coronal mass ejection's (or flux rope's) upward motion via the impulsive magnetic reconnection process. The magnitude of impulsive magnetic reconnection rate and the magnetic reconnection electric field at the reconnecting X-line can be computed from the rate of change in magnetic flux swept by the evolution of H- alpha ribbons or EUV ribbons or HXR footpoints. By averaging the magnetic flux change rate over the ribbons the peak reconnection electric field during the HXR impulsive phase is ~ 1 kV/m for X-class flares. Further studies show that the magnetic flux change rate of reconnected field lines varies along the ribbons and the peak value is located near the HXR footpoint and can be several times larger than the averaged value. However, solar flare observations provide "indirect" measurement of impulsive reconnection. In this paper we also report results of recent laboratory experiments performed at the University of Tokyo that directly observed and measured the impulsive magnetic reconnection process associated with accelerated ejection of flux ropes. The combined results from both solar observations and laboratory plasma experiments thus provide a much stronger support of the impulsive magnetic reconnection theory for explaining impulsive phenomena in solar flares and CMEs.
Cheng Chung-Chieh
Choe G.
Ono Yohei
Yang Yadong
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