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αΛ-dynamos

Published online by Cambridge University Press:  12 April 2016

A. Brandenburg ,
D. Moss ,
M. Rieutord ,
G. Rüdiger  and
I. Tuominen
A. Brandenburg
Affiliation:
Observatory and Astrophysics Laboratory, University of Helsinki, Tähtitorninmäki, SF-00130 Helsinki, Finland NORDITA, Blegdamsvej 17, DK-2100 Copenhagen, Denmark
D. Moss
Affiliation:
Dept. of Mathematics, The University, Manchester M13 9PL, UK
M. Rieutord
Affiliation:
Observatoire de Toulouse, 14 av. E. Belin, F-31400 Toulouse, France
G. Rüdiger
Affiliation:
Astrophysikalisches Observatorium Potsdam, O-1560 Potsdam, FRG
I. Tuominen
Affiliation:
Observatory and Astrophysics Laboratory, University of Helsinki, Tähtitorninmäki, SF-00130 Helsinki, Finland

Abstract

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In contrast to αω-dynamos, where the angular velocity is arbitrarily prescribed, we consider here αΛ-dynamos, for which the differential rotation and meridional circulation are solutions of the momentum equation. The non-diffusive parts of the Reynolds stress tensor are parameterized by the Λ-effect. In earlier investigations we have shown that the turbulent magnetic diffusivity has to be much smaller than the eddy viscosity, otherwise the dynamo is not oscillatory or else the contours of constant angular velocity are cylindrical, contrary to observations. In the present paper we investigate the effects of compressibility.

Type
Part II Current stellar dynamo theory
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 147 - 150
Copyright
Copyright © Springer-Verlag 1991

References

Brandenburg, A., Moss, D., Rüdiger, G., Tuominen, I.: 1990, Solar Physics 128, 243 (Paper I)Google Scholar
Gilman, P.A., Miller, J.: 1981, Astrophys. J. Suppl. 46, 211 CrossRefGoogle Scholar
Glatzmaier, G.A.: 1985, Astrophys. J. 291, 300 Google Scholar
Rüdiger, G.: 1989, Differential rotation and Stellar Convection: Sun and solar-type stars, Gordon and Breach, New York Google Scholar