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Role of longitudinal activity complexes for solar and stellar dynamos

Published online by Cambridge University Press:  18 July 2013

Maarit J. Mantere ,
Petri J. Käpylä  and
Jaan Pelt
Maarit J. Mantere
Affiliation:
Department of Physics, PO Box 64, FI-00014University of Helsinki, Finland Department of Information and Computer Science, Aalto University, PO Box 15400, FI-00076 Aalto, Finland
Petri J. Käpylä
Affiliation:
Department of Physics, PO Box 64, FI-00014University of Helsinki, Finland Nordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden
Jaan Pelt
Affiliation:
Tartu Observatory, Tõravere, 61602, Estonia
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Abstract

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In this paper we first discuss observational evidence of longitudinal concentrations of magnetic activity in the Sun and rapidly rotating late-type stars with outer convective envelopes. Scenarios arising from the idea of rotationally influenced anisotropic convective turbulence being the key physical process generating these structures are then presented and discussed - such effects include the turbulent dynamo mechanism, negative effective magnetic pressure instability (NEMPI) and hydrodynamical vortex instability. Finally, we discuss non-axisymmetric stellar mean-field dynamo models, the results obtained with them, and compare those with the observational information gathered up so far. We also present results from a pure α2 mean-field dynamo model, which show that time-dependent behavior of the dynamo solutions can occur both in the form of an azimuthal dynamo wave and/or oscillatory behavior related to the alternating energy levels of the active longitudes.

Keywords

MHD – turbulence – Sun: magnetic fields – Stars: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S294: Solar and Astrophysical Dynamos and Magnetic Activity , August 2012 , pp. 175 - 186
Copyright
Copyright © International Astronomical Union 2013 

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