Modelling the influence of photospheric turbulence on solar flare statistics

TL;DR

This paper models how photospheric turbulence influences solar flare statistics, explaining scale-free energy distributions and long-range correlations through flux tube interactions and turbulence effects, aligning well with satellite data.

Contribution

It introduces a model linking photospheric turbulence and flux tube interactions to solar flare statistics, providing a physical basis for observed scale-free and correlated behaviors.

Findings

Scale-free energy distribution explained by photospheric vorticity.

Long-range correlations arise from flux tube interactions.

Model shows good agreement with satellite measurements.

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.