HR: 08:00h
AN: SH11C-01    [Abstracts]
TI: Flaring capability of solar active regions versus their magnetic power spectra: observational aspects
AU: * Abramenko, V
EM: avi@bbso.njit.edu
AF: Big Bear Solar Observatory, New Jersey Institute of Technology, 40386 North Shore Lane, Big Bear City, CA 92314 United States
AB: Spatio-temporal dynamics of magnetic flux tubes in the photosphere and beneath is thought to be a driving mechanism for energy built-up and energy release phenomena in the solar atmosphere. We calculated magnetic power spectra from high-resolution SoHO/MDI magnetograms for 16 active regions and revealed that non-flaring active regions possess Kolmogorov-type spectra, whereas active regions that launched X-class flares display much steeper, non-Kolmogorov spectra. Moreover, the non-Kolmogorov spectrum was observed since the very beginning of the emergence of flaring active regions. The Kolmogorov-type spectra that was found in non-flaring active regions might suggest a nearly stationary turbulent regime when the dynamical equilibrium between the energy input at large scales and energy output at small scales provides premises for a smooth evolution without catastrophes. On the other hand, the non-Kolmogorov spectra of flaring active regions imply the inhomogeneous non-stationary turbulence regime when the dissipation of energy might occur in a catastrophe-like manner (flares). We will also discuss an implication of our findings to the problem of the energy build-up in solar eruptions.
UR: http://www.bbso.njit.edu/~avi
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: Fall Meeting 2005