Abstract
AbstractThe motivation for considering distributed large scale dynamos in the solar context is reviewed in connection with the magnetic helicity constraint. Preliminary accounts of 3‐dimensional direct numerical simulations (in spherical shell segments) and simulations of 2‐dimensional mean field models (in spherical shells) are presented. Interesting similarities as well as some differences are noted. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
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