The chromospheric response due to filament eruption
Received 4 October 1996 / Accepted 12 December 1996
Frozen-in motion of chromospheric plasma during an eruption of a filament of inverse polarity is considered. At the initial stage of the filament ascent, magnetic field compresses the chromospheric plasma within two belts disposed bilaterally along a polarity inversion line. Compression should be accompanied by heating of plasma and enhancement of emission in H . The distance between the belts increases as the filament ascends. The estimates show that this mechanism can be effective to represent the H flare kernels dynamics in two-ribbon flares.
Key words: Sun: chromosphere Sun: filaments Sun: magnetic fields
Send offprint requests to: B.P. Filippov
© European Southern Observatory (ESO) 1997
Online publication: May 26, 1998