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The Role of Overshoot in Solar Activity: A Direct Simulation of the Dynamo

Published online by Cambridge University Press:  12 April 2016

A. Brandenburg ,
R.L. Jennings ,
Å. Nordlund ,
R.F. Stein  and
I. Tuominen
A. Brandenburg
Affiliation:
Observatory and Astrophysics Laboratory, University of Helsinki, Finland NORDITA, Blegdamsvej 17, DK-2100 Copenhagen, Denmark
R.L. Jennings
Affiliation:
Dept. of Appl. Math. and Theor. Physics, Cambridge CB3 9EW, UK
Å. Nordlund
Affiliation:
Copenhagen University Observatory, DK-1350 Copenhagen K, Denmark
R.F. Stein
Affiliation:
Dept. of Physics and Astronomy, Michigan State University, USA
I. Tuominen
Affiliation:
Observatory and Astrophysics Laboratory, University of Helsinki, Finland

Abstract

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We investigate convective overshoot in a layer of electrically conducting fluid. The radiative conductivity is assumed to be larger in the lower part of the layer which makes it stable to convective motions, yet penetrative convection from the upper layer can occur. The numerical resolution is 633 gridpoints. We observe a dynamo effect for magnetic Reynolds numbers around one thousand when a magnetic seed field is rapidly concentrated to form flux tubes. Later the average magnetic field is expelled from the convectively unstable regions, but it accumulates in the interface between the convection zone and the radiative interior.

Type
Part I Convection and turbulence as the basis of magnetic activity
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 86 - 88
Copyright
Copyright © Springer-Verlag 1991

References

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