Flare ribbon pixels in 10 solar flares show power-law distributions for waiting time and duration, but not for peak intensity, energy, or magnetic field strength, only partly matching self-organized criticality predictions.
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Size Distributions of Arcsecond-Scale Properties of Solar Flare Ribbons
Flare ribbon pixels in 10 solar flares show power-law distributions for waiting time and duration, but not for peak intensity, energy, or magnetic field strength, only partly matching self-organized criticality predictions.