Mathematics
Scientific paper
Aug 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985stin...8630622f&link_type=abstract
Presented at the NSO/SMM Summer Workshop, Sacramento, Calif., 1 Aug. 1985
Mathematics
Brightness, Chromosphere, Coronal Loops, Shock Waves, Solar Flares, Deposition, Equations Of Motion, Mathematical Models
Scientific paper
Rapid energy release (by either thick target (beam) or thermal models of heating) in solar flare loop models usually leads to chromospheric evaporation, the process of heating cool chromospheric material to coronal temperatures, and the resulting increase in hot soft x-ray emitting plasma. The evaporated plasma flows up into the coronal portion of the loop because of the increased pressure in the evaporated region. However, the pressure increase also leads to a number of interesting phenomena in the flare chromosphere. The sudden pressure increase in the evaporated plasma initiates a downward moving chromospheric condensation, an overdense region which gradually decelerates as it accretes material and propagates into the gravitationally stratified chromosphere. Solutions to an equation of motion for this condensation shows that its motion decays after about one minute of propagation into the chromosphere. When the front of this downflowing region is supersonic relative to the atmosphere ahead of it, a radiating shock will form. If the downflow is rapid enough, the shock strength should be sufficient to excite UV radiation normally associated with the transition region, and furthermore, the radiating shock will be brighter than the transition region. These results lead to a number of observationally testable relationships between the optical and ultraviolet spectra from the condensation and radiating shock.
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