Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.2913r&link_type=abstract
American Astronomical Society Meeting 210, #29.13; Bulletin of the American Astronomical Society, Vol. 39, p.139
Astronomy and Astrophysics
Astronomy
Scientific paper
What is the role magnetic helicity plays in solar eruptions? To find out, we calculate the magnetic helicity flux for 48 X-class flaring solar active regions and for 345 M-class flaring regions. Each region was observed over a period of a few, to several, days by SoHO/MDI. We find consistently higher helicity buildup rates for the X-flaring regions. X-class flares do not occur if the peak helicity flux is smaller than 6 x 1036 Mx2/s, with most nonflaring regions showing much smaller peaks. The weak hemispheric preference of magnetic
helicity is caused by the solar differential rotation, but it is blurred by the intrinsic helicity injection which is more disorganized and of opposite sign. Notably, X-flaring regions can generate the helicity for a typical CME within a few hours to a few days, contrary to most flare-quiescent regions that require from several tens to hundreds of days. We conclude that accumulation of magnetic helicity is a precondition for major flare/CME events. This work has received partial support by NASA Grants NAG5-13504 and NNG05-GM47G.
Georgoulis Manolis K.
Rust David Maurice
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