Two-ribbon H-alpha emission during the eruption of a filament

Details Two-ribbon H-alpha emission during the eruption of a filament Two-ribbon H-alpha emission during the eruption of a filament

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997azh....74..635f&link_type=abstract

Astronomicheskij Zhurnal, vol. 74, p. 635

Astronomy and Astrophysics

Astronomy

Solar Spectra, H Alpha Line, Emission Spectra, Chromosphere, Plasma Dynamics, Solar Magnetic Field, Magnetic Field Configurations, Filaments, Polarity, Astronomical Models, Solar Flares

Scientific paper

Frozen-in motions of chromospheric plasma during the eruption of a filament, with a magnetic field configuration described by an inverse-polarity model, are considered. When the filament begins its motion, the field compresses the chromospheric gas within two bands located symmetrically with respect to the neutral line dividing the polarities. The compression is accompanied by heating of the plasma and enhanced H-alpha emission. As the filament rises above the chromosphere, the band separation grows. Estimates indicate that this mechanism may be able to describe the dynamics of H-alpha emission sites in two-ribbon flares.

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