Other
Scientific paper
Aug 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987esasp.275....3f&link_type=abstract
In ESA, Proceedings of the 21st ESLAB Symposium on Small Scale Plasma Processes in the Solar Chromosphere/Corona, Interplanetary
Other
1
Coronal Loops, Magnetic Field Configurations, Magnetic Field Reconnection, Solar Flares, Solar Magnetic Field, Solar X-Rays, Chromosphere, Plasma Heating, Shock Heating, Solar Radiation
Scientific paper
Reconnection models of the main phase of large solar flares are used to explain the energetics and the motions of the large flare loops that occur during this phase. Correct predictions for the density and temperature of the X-ray emitting loops are obtained by coupling magnetic reconnection with chromospheric ablation. In the reconnection models the ablation is driven by the thermal conduction of heat along magnetic field lines connecting the reconnection shocks in the corona with the flare ribbons in the chromosphere. Combining the compressible reconnection theory of Soward and Priest (1982) with the magnetohydrodynamic (MHD) subshock criteria of Coroniti (1970) shows that the Petschek-type slow-mode shocks in the vicinity of the x-line always dissociate into pairs of isothermal slow-mode subshocks and thermal conduction fronts. The rate of expansion of the loops is a function of the reconnection rate, and loops can be evolving self-similarly in time with their height increasing as sq root t and the reconnection rate decreasing as t to the minus 1.
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