Modelling the influence of photospheric turbulence on solar flare statistics

M. Mendoza (), A. Kaydul, L. de Arcangelis, J. S. Andrade and H. J. Herrmann
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M. Mendoza: ETH Zürich, Computational Physics for Engineering Materials, Institute for Building Materials
A. Kaydul: ETH Zürich, Computational Physics for Engineering Materials, Institute for Building Materials
L. de Arcangelis: Second University of Naples and CNISM
J. S. Andrade: Universidade Federal do Ceará
H. J. Herrmann: ETH Zürich, Computational Physics for Engineering Materials, Institute for Building Materials

Nature Communications, 2014, vol. 5, issue 1, 1-8

Abstract: Abstract Solar flares stem from the reconnection of twisted magnetic field lines in the solar photosphere. The energy and waiting time distributions of these events follow complex patterns that have been carefully considered in the past and that bear some resemblance with earthquakes and stockmarkets. Here we explore in detail the tangling motion of interacting flux tubes anchored in the plasma and the energy ejections resulting when they recombine. The mechanism for energy accumulation and release in the flow is reminiscent of self-organized criticality. From this model, we suggest the origin for two important and widely studied properties of solar flare statistics, including the time–energy correlations. We first propose that the scale-free energy distribution of solar flares is largely due to the twist exerted by the vorticity of the turbulent photosphere. Second, the long-range temporal and time–energy correlations appear to arise from the tube–tube interactions. The agreement with satellite measurements is encouraging.

Date: 2014
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DOI: 10.1038/ncomms6035

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