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Published online by Cambridge University Press: 11 May 2010
The detailed dynamics of the Solar dynamo presents a significant challenge to our understanding of the interaction of convection and magnetic fields in the Solar interior. In this paper we discuss certain aspects of this interaction, such as modification of convective energy transport, and turbulent dissipation of magnetic fields. The latter controls the spatial distribution of the magnetic field and its time dependence. We also discuss how these results may influence current Solar dynamo calculations.
MOTIVATION
Solar activity manifests itself in many forms but perhaps most importantly through the presence of a magnetic field. The topic of this meeting is that of dynamos, in Solar and planetary contexts. In the case of the Sun the dynamo, which seems likely to be responsible for at least part of the Solar activity we observe, acts on a global scale. That is, the period of the dynamo is 22 years (a timescale distinct from those usually encountered on the Sun), sunspots appear within latitude bands and their numbers (in terms of monthly or yearly running means) increase and decrease over one cycle. There is however, a strong asymmetry of the Solar cycle in time, i.e. the growth phase is shorter (and dependent of the amount of activity) than the decay, or descending phase. In addition, the polar field of the Sun is observed to reverse around Solar maximum, again with a distinct asymmetry between hemispheres. Despite these global-scale features, the Solar magnetic field has many spatial components (Stenflo 1991) and the majority of the magnetic flux appears in small elements.
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