Volume 591, July 2016
|Number of page(s)||9|
|Published online||09 June 2016|
The turbulent diffusion of toroidal magnetic flux as inferred from properties of the sunspot butterfly diagram
Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
Received: 1 September 2015
Accepted: 21 April 2016
Context. In order to match observed properties of the solar cycle, flux-transport dynamo models require the toroidal magnetic flux to be stored in a region of low magnetic diffusivity, typically located at or below the bottom of the convection zone.
Aims. We infer the turbulent magnetic diffusivity affecting the toroidal field on the basis of empirical data.
Methods. We considered the time evolution of mean latitude and width of the activity belts of solar cycles 12–23 and their dependence on cycle strength. We interpreted the decline phase of the cycles as a diffusion process.
Results. The activity level of a given cycle begins to decline when the centers of its equatorward propagating activity belts come within their (full) width (at half maximum) from the equator. This happens earlier for stronger cycles because their activity belts are wider. From that moment on, the activity and the belt width decrease in the same manner for all cycles, independent of their maximum activity level. In terms of diffusive cancellation of opposite-polarity toroidal flux across the equator, we infer the turbulent diffusivity experienced by the toroidal field, wherever it is located, to be in the range 150–450 km2 s-1. Strong diffusive latitudinal spreading of the toroidal flux underneath the activity belts can be inhibited by an inflow toward the toroidal field bands in the convection zone with a magnitude of several meters per second.
Conclusions. The inferred value of the turbulent magnetic diffusivity affecting the toroidal field agrees, to order of magnitude, with estimates based on mixing-length models for the solar convection zone. This is at variance with the requirement of flux-transport dynamo models. The inflows required to keep the toroidal field bands together before they approach the equator are similar to the inflows toward the activity belts observed with local helioseismology.
Key words: Sun: magnetic fields / Sun: activity
© ESO, 2016
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