Physics
Scientific paper
Aug 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...98..267d&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 98, Aug. 1985, p. 267-280.
Physics
25
Ablation, Atmospheric Heating, Chromosphere, Solar Flares, Electron Beams, Electron Energy, Solar Maximum Mission
Scientific paper
Based on observations of two flares by the Solar Maximum Mission, a quantitative model of the solar flare footpoint and its evolution is presented. The particle numbers and energies involved in the processes of heating, ablation, and convection are discussed. In the model, the kernel is heated by electron beams from above. Medium and high energy electrons penetrating down to the top of the chromosphere cause heating of the chromospheric gas to about 50 MK and ablation, leading to the abrupt formation of a superhot flare kernel and a likely superhot 'dome' above it through which gas rises up and spreads out convectively. The heating process lasts only for a few minutes. The difference between the Doppler temperature and the electron temperature derived from line intensity ratios or from low energy count rate ratios is ascribed to truncation of the tail of the electron energy distribution in the kernel.
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