Astronomy and Astrophysics – Astronomy
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21632103a&link_type=abstract
American Astronomical Society, AAS Meeting #216, #321.03; Bulletin of the American Astronomical Society, Vol. 41, p.912
Astronomy and Astrophysics
Astronomy
Scientific paper
Solar photosphere is in a state of highly developed turbulence owing to the sub-photospheric convection. The strength and growth of turbulence determines eventually the degree of complexity of the magnetic field. Complexity is thought to be responsible for the flaring productivity of an active region (AR). Due to the inherently non-linear nature of turbulence, complexity hardly can be adequately presented by a single scalar parameter. Rather a spectrum of values representing the behavior of the field at different scales should be analyzed. Here the results of analysis of the magnetic energy spectra and intermittency spectra for 186 ARs observed during 2000-2006 with SOHO/MDI in the high-resolution mode are presented. We thus found that steeper energy spectra are related to higher flaring productivity (the correlation coefficient CC=0.69). The intermittency spectrum was determined via a hyper flatness function (ratio of the 6th-order structure function to the squared 3rd-order structure function) for a set of spatial scales. It was found that the range of scales where the hyper-flatness decreases (a signature of intermittency and multifractality) can vary for different ARs, however, there is a strong tendency for ARs with higher flare productivity to posses steeper and broader intermittency spectrum at small scales (below 10-20 Mm). Very steep and broad intermittency spectra found for several ARs showing extremely high flaring activity seem to be related to shredded magnetic fields along the neutral line of a delta-structure. Our results indicate that the capability of an active region to produce solar flares is directly related to the development of intermittent structures in an active region magnetic field. Prospects of applying this approach to new high resolution data from Hinode, SDO and NST acquired during the oncoming solar maximum will be also discussed.
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