Fine structure of solar filaments. II - Dynamics of threads and footpoints

Details Fine structure of solar filaments. II - Dynamics of threads and footpoints Fine structure of solar filaments. II - Dynamics of threads and footpoints

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...252..353s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 252, no. 1, Dec. 1991, p. 353-365. Research supported by Observatoire de Paris

Astronomy and Astrophysics

Astrophysics

63

Chromosphere, Magnetic Field Configurations, Solar Activity, Solar Magnetic Field, Solar Prominences, Astronomical Spectroscopy, Doppler Effect, Faculae, H Alpha Line, Solar Atmosphere, Solar Granulation

Scientific paper

The dynamical behavior of the fine structures observed at the Pic du Midi through a multichannel subtractive double pass (MSDP) spectrograph during a 15-min period has been studied. Widespread continual changes in the velocity field were observed during this period, and, for the whole region, there was virtually no correlation from one minute to the next. High velocities (up to +/-15 km/s) were detected at locations where the filament was anchored in the chromosphere using the first order differential cloud model. It is argued that these footpoints are essentially the same kind of structures as the chromospheric bushes seen around supergranules, which show spiculelike activity modified by the local magnetic field geomentry. Parallel to the filament axis elongated Doppler structures with coherent motions were observed. These structures may be interpreted as magnetic flux tubes identifiable during their short rise time, or they may indicate that there are coherent wave motions.

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