Scale-Free Magnetic Networks: Comparing Observational Data with a Self-Organizing Model of the Coronal Field

Details Scale-Free Magnetic Networks: Comparing Observational Data with a Self-Organizing Model of the Coronal Field Scale-Free Magnetic Networks: Comparing Observational Data with a Self-Organizing Model of the Coronal Field

2003-09-08

arxiv.org/abs/astro-ph/0309230v1

Astronomy and Astrophysics

Astrophysics

16 pages, 11 figures

Scientific paper

We propose that the coronal magnetic field, linking concentrations on the photosphere through an interwoven web of flux, embodies a scale-free network. It arises from a self-organized critical dynamics including flux emergence, the diffusion and merging of magnetic concentrations, as well as avalanches of reconnecting flux tubes. Magnetic concentrations such as fragments, pores and sunspots, are `nodes' joined by flux tubes or `links'. The number of links emanating from a node is scale-free. We reanalyze the quiet-Sun data of Close et al and show that the distribution of magnetic concentration strengths is a power law with an index $\gamma= 1.7 \pm 0.3$, over the entire range of the measurement, about $(2-500)\times 10^{17}$ Mx. This distribution is compatible with that for the sizes of active regions reported by Harvey and Schwaan. Thus magnetic concentrations may be scale-free from the smallest measurable fragments to the large active regions. Numerical simulations of a self-organized critical model give the same index $\gamma$, within statistical uncertainty. The exponential distribution of flux tube lengths also agrees quantitatively with results from the model. Calibration with the measured diffusion constant of magnetic concentrations allows us to calculate a flux turnover time in the model to be of order 10 hours and the total solar flux to be of order $10^{23}$Mx, agreeing with observations. We introduce two other statistical quantities to characterize scale-free networks. The probability distribution for the amount of flux connecting a pair of concentrations, and the number of distinct concentrations linked to a given one are predicted to be scale-free, with different indices. Our approach unifies the observation of scale free flare energies with the coronal magnetic field structure.

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