Solar Coronal Magnetic Filaments: The Roll Effect in Erupting Prominences

Details Solar Coronal Magnetic Filaments: The Roll Effect in Erupting Prominences Solar Coronal Magnetic Filaments: The Roll Effect in Erupting Prominences

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.0508b&link_type=abstract

American Astronomical Society, SPD meeting #34, #05.08; Bulletin of the American Astronomical Society, Vol. 35, p.815

Astronomy and Astrophysics

Astronomy

Scientific paper

Based on observations, we suggest that the magnetic field of a filament (or prominence) should be treated as a ribbon. We then use the ribbon hypothesis to explain an observable effect which we term the roll effect. Briefly, the nature of the roll effect is manifested by a filament ribbon in its slow pre-eruptive rise through the tendency to be non-radial, with a small preferential roll in one direction. When it erupts and further rises, the most elevated portion bends over in the roll direction and is forced to become nearly horizontal. Propagation of the roll down the legs of the filament twists them in opposite directions as we verify in observed examples. The direction of this rolling has a one-to-one correspondence with the combination of filament chirality that is known to be in one-to-one correspondence with the polarity of the photospheric magnetic field on either side of the filament. Because the rolling can occur in only two possible forms of handedness, they constitute an observable form of chirality specific to erupting filaments. Establishing this bijection is the major concern of this talk.
The contribution of PDB was partially supported by a Valerie Mysercough Prize, SFM was supported by NASA grant NAG5-5917 and MAB gratefully acknowledges funding by PPARC grant PPA/G/S/1999/00059.

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