2-RIBBON H-ALPHA-EMISSION DURING THE ERUPTION OF A FILAMENT

Frozen-in motions of chromospheric plasma during the eruption of a fil ament with a magnetic field configuration described by an inverse-pola rity model are considered. When the filament begins its motion, the fi eld compresses the chromospheric gas within two bands located symmetri cally with respect to the neutral line dividing the polarities. The co mpression is accompanied by heating of the plasma and enhanced H alpha emission. As the filament rises above the chromosphere, the band sepa ration grows. Estimates indicate that this mechanism may be able to de scribe the dynamics of sites of Ha in two-ribbon flares.