Mathematics – Dynamical Systems
Scientific paper
Oct 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.505..105v&link_type=abstract
In: SOLMAG 2002. Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188, 11 - 15 Jun
Mathematics
Dynamical Systems
3
Convection Zone, Active Regions, Flares, Coronal Heating
Scientific paper
We are making an attempt to associate the formation and evolution of active regions with the heating and flaring of the plasmas in the solar atmosphere above the active region. The working hypothesis in our review is that "active regions are open dynamical systems away from equilibrium, driven by the turbulent convection zone". New magnetic loops emerge from the convection zone and are subject to surface diffusion (random motion), which leads to cancellation of magnetic energy when they collide with magnetic structures of opposite polarity. In the course of their evolution from birth to disappearance, active regions reach quickly the stage of Self-Organized Criticality (SOC), heat the corona by driving nano-flares, micro-flares and flares. We believe that the statistical properties of the active regions at the photosphere (size distribution, fractal dimension etc.) are correlated with the statistical properties of all aspects of solar activity (Ellerman Bombs, Bright Points, flares, particle acceleration, etc.). Surprisingly, all these phenomena share one common characteristic, they are self-similar and their statistical behaviour follows well defined power laws. This last point reinforces our belief that the solar atmosphere is coupled, through the magnetic field, with the convection zone, which drives all the observed activity at the photosphere, chromosphere, corona and interplanetary space.
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