HR: 16:00h
AN: SH14B-01 INVITED    [Abstracts]
TI: Quantifying turbulence in solar magnetic fields: can this help predict solar eruptions?
AU: * Georgoulis, M K
EM: manolis.georgoulis@jhuapl.edu
AF: Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723, United States
AB: 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.
DE: 7519 Flares
DE: 7524 Magnetic fields
DE: 7529 Photosphere
DE: 7863 Turbulence (4490)
DE: 7924 Forecasting (2722)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting