Twisting motions in a disturbed solar filament

Details Twisting motions in a disturbed solar filament Twisting motions in a disturbed solar filament

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...142..249s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 142, no. 2, Jan. 1985, p. 249-255. Research supported by the Institut National

Astronomy and Astrophysics

Astrophysics

24

Coronal Loops, Magnetohydrodynamics, Solar Magnetic Field, Solar Oscillations, Solar Prominences, Stellar Spectrophotometry, Doppler Effect, H Alpha Line, Twisting

Scientific paper

Time sequences of the vertical velocity field in a disturbed solar active region filament (AR 2646) have been derived using the MSDP spectrograph operating in Hα at the Meudon Solar Tower. Following a period of systematic upward velocities a pair of closely aligned elongated regions of oppositely directed velocities develops and persists over several minutes. These velocities are interpreted in terms of a twisted magnetic flux rope model for the filament. The initial upward motions indicate that the flux rope is rising. This should lead to an expansion since the surrounding pressure is decreasing with height. Conservation of the current and the magnetic flux along the filament then requires twisting motions as the flux rope adjusts to a new radial equilibrium when rising into the corona.

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