Physics
Scientific paper
Feb 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..143..247s&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 143, no. 2, p. 247-258.
Physics
Electron Acceleration, H Alpha Line, Plasma Heating, Solar Electrons, Solar Flares, Solar Physics, Beta Factor, Magnetohydrodynamic Stability
Scientific paper
For the flares analyzed, nonthermal electron signatures in H alpha are never cospatial with regions of maximum current density. In order to observe nonthermal electron signatures in H alpha, the plasma beta in the acceleration region must be no greater than 0.3, the energy flux of electrons above 20 keV must be greater than 10 exp 10 erg/sq cm per sec, the column density between the electron source and the chromosphere must not be greater than 10 exp 20 sq cm, and the coronal pressure in the flux tube connecting to the H alpha layer must be less than or equal to 100 dyne/sq cm. A suitable energy flux of electrons is most easily found in the initial stages of flares. In contrast, a coronal pressure of 1000 dyne/sq cm is the only condition needed for high-pressure H alpha signatures. Consequently, high-pressure signatures may be expected to occur more frequently and generally later in time than nonthermal electron signatures.
Hénoux Jean-Claude
Smith Donelson F.
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