The chromospheric response due to filament eruption.

Details The chromospheric response due to filament eruption. The chromospheric response due to filament eruption.

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...324..324f&link_type=abstract

Astronomy and Astrophysics, v.324, p.324-328

Astronomy and Astrophysics

Astrophysics

5

Sun: Chromosphere, Sun: Filaments, Sun: Magnetic Fields

Scientific paper

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 Hα. The distance between the belts increases as the filament ascends. The estimates show that this mechanism can be effective to represent the Hα flare kernels dynamics in two-ribbon flares.

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