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Title:
Paradigm shifts in solar dynamo modeling
Authors:
Brandenburg, Axel
Affiliation:
AA(Nordita, Roslagstullsbacken 23, 10691 Stockholm, Sweden)
Publication:
Cosmic Magnetic Fields: From Planets, to Stars and Galaxies, Proceedings of the International Astronomical Union, IAU Symposium, Volume 259, p. 159-166
Publication Date:
04/2009
Origin:
CUP
Keywords:
MHD, turbulence, Sun: coronal mass ejections (CMEs), Sun: magnetic fields
DOI:
10.1017/S1743921309030403
Bibliographic Code:
2009IAUS..259..159B

Abstract

Selected topics in solar dynamo theory are being highlighted. The possible relevance of the near-surface shear layer is discussed. The role of turbulent downward pumping is mentioned in connection with earlier concerns that a dynamo-generated magnetic field would be rapidly lost from the convection zone by magnetic buoyancy. It is argued that shear-mediated small-scale magnetic helicity fluxes are responsible for the success of some of the recent large-scale dynamo simulations. These fluxes help in disposing of excess small-scale magnetic helicity. This small-scale magnetic helicity, in turn, is generated in response to the production of an overall tilt in each Parker loop. Some preliminary calculations of this helicity flux are presented for a system with uniform shear. In the Sun the effects of magnetic helicity fluxes may be seen in coronal mass ejections shedding large amounts of magnetic helicity.
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