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From convective to stellar dynamos

Published online by Cambridge University Press:  12 August 2011

Axel Brandenburg ,
Petri J. Käpylä  and
Maarit J. Korpi
Axel Brandenburg
Affiliation:
NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden Department of Astronomy, Stockholm University, SE-10691 Stockholm, Sweden
Petri J. Käpylä
Affiliation:
NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden Department of Physics, PO Box 64, FI-00014 University of Helsinki, Finland
Maarit J. Korpi
Affiliation:
Department of Physics, PO Box 64, FI-00014 University of Helsinki, Finland
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Abstract

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Convectively driven dynamos with rotation generating magnetic fields on scales large compared with the scale of the turbulent eddies are being reviewed. It is argued that such fields can be understood as the result of an α effect. Simulations in Cartesian domains show that such large-scale magnetic fields saturate on a time scale compatible with the resistive one, suggesting that the magnitude of the α effect is here still constrained by approximate magnetic helicity conservation. It is argued that, in the absence of shear and/or any other known large-scale dynamo effects, these simulations prove the existence of turbulent α2-type dynamos. Finally, recent results are discussed in the context of solar and stellar dynamos.

Keywords

MHD – turbulence – Sun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 279 - 287
Copyright
Copyright © International Astronomical Union 2011

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