Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh14b..01g&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SH14B-01
Physics
7519 Flares, 7524 Magnetic Fields, 7529 Photosphere, 7863 Turbulence (4490), 7924 Forecasting (2722)
Scientific paper
Magnetic fields in solar active regions present us with a beautiful, although inextricable, complexity, and undergo dynamical evolution that is often far from predictable. This behavior is commonly attributed to the inherently turbulent, filamentary nature of magnetic fields in the solar atmosphere. We ask whether this turbulence and its manifestations can help us predict solar eruptions. To this purpose, we briefly outline the physical relationship between turbulence and (critical) self-organization, as well as their phenomenology, such as spatiotemporal intermittency, self-similar fragmentation, fractality, and multifractality of solar active-region magnetic fields. We also review the array of techniques that have been recently implemented to quantify these turbulent features and we apply them to numerous flaring and nonflaring active regions aiming toward quantitative flare prediction. Results and conclusions are presented in hopes to intrigue and stimulate further discussion on this fascinating, clearly outstanding, problem.
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