Physics
Scientific paper
Jun 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...78..229p&link_type=abstract
Solar Physics, vol. 78, June 1982, p. 229-241.
Physics
26
Coronal Loops, Ohmic Dissipation, Solar Flares, Solar Flux Density, Solar Magnetic Field, Solar X-Rays, Magnetic Field Configurations, Magnetic Flux, Resistance Heating, Skylab Program, Solar Prominences, Temporal Distribution, Thermal Energy
Scientific paper
A quantitative model for the basic energy release process occurring in two-ribbon solar flares is presented and compared with observations. Eruptions are shown to occur 15 min before flare onset, caused by reconnection of locally open magnetic field lines as the prominences align along the photospheric magnetic field neutral lines. The prominences actually cause a disruption of the field lines, forcing them outward until reconnection happens during the flare. Post-flare loops are noted to rarely become visible, having to necessarily climb into the corona first. The process is modeled as an effect of Joulean heating caused by connection in a rising loop system. Particular attention is given to the temporal evolution of the thermal energy density at the top of the loops. Comparisons are made of the model predictions with three observed flare events using different magnetic geometries. The calculated energy density is demonstrated to follow the same curve as the observed densities.
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