Physics
Scientific paper
Jul 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..146..137r&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 146, no. 1, p. 137-145.
Physics
9
H Alpha Line, Magnetic Field Configurations, Solar Flares, Solar Magnetic Field, Solar Prominences, Magnetic Field Reconnection, Shear Layers, Spectroheliographs, Umbras
Scientific paper
We have analyzed the variations in shear angle over a time interval of 30 s during a flare on June 11, 1991, using Kodaikanal Observatory spectroheliogram and photoheliogram data, and assuming H-alpha filaments are a proxy for the neutral lines. The changes in shear angles have been analyzed at two points of the filament. The orientation of the H-alpha filament underwent a considerable change of about 55 deg from June 10, 1991 to prior to the start of the flare on June 11, 1991. The photoheliogram on June 10, 1991 shows considerable twisting of the umbrae (in one common penumbra) and broke into parts before the onset of the flare on June 11, 1991. The twisting of umbrae on June 10, 1991 shows that sunspot proper motion plays an important role in bringing a non-potential character to the field lines. This in turn develops shear and kink and it is argued that changes in filament orientation over a small interval of a half minute triggers the eruption of the flare.
Aleem S. M. P.
Rausaria R. R.
Singh Jagdev
Sundara Raman K.
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