Astronomy and Astrophysics – Astronomy
Scientific paper
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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