Flaring capability of solar active regions versus their magnetic power spectra: observational aspects

Details Flaring capability of solar active regions versus their magnetic power spectra: observational aspects Flaring capability of solar active regions versus their magnetic power spectra: observational aspects

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh11c..01a&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH11C-01

Other

7519 Flares, 7524 Magnetic Fields, 7529 Photosphere, 7863 Turbulence (4490), 7924 Forecasting (2722)

Scientific paper

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.

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