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The small-scale magnetic field is ubiquitous at the solar surface---even athigh latitudes. From observations we know that this field is uncorrelated (orperhaps even weakly anticorrelated) with the global sunspot cycle. Our aim isto explore the origin, and particularly the cycle dependence of such aphenomenon using three-dimensional dynamo simulations. We adopt a simple modelof a turbulent dynamo in a shearing box driven by helically forced turbulence.Depending on the dynamo parameters, large-scale (global) and small-scale(local) dynamos can be excited independently in this model. Based onsimulations in different parameter regimes, we find that, when only thelarge-scale dynamo is operating in the system, the small-scale magnetic fieldgenerated through shredding and tangling of the large-scale magnetic field ispositively correlated with the global magnetic cycle. However, when bothdynamos are operating, the small-scale field is produced from both thesmall-scale dynamo and the tangling of the large-scale field. In thissituation, when the large-scale field is weaker than the equipartition value ofthe turbulence, the small-scale field is almost uncorrelated with thelarge-scale magnetic cycle. On the other hand, when the large-scale field isstronger than the equipartition value, we observe an anticorrelation betweenthe small-scale field and the large-scale magnetic cycle. This anticorrelationcan be interpreted as a suppression of the small-scale dynamo. Based on ourstudies we conclude that the observed small-scale magnetic field in the Sun isgenerated by the combined mechanisms of small-scale dynamo and tangling of thelarge-scale field.

Is the small-scale magnetic field correlated with the dynamo cycle?