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Convective mechanism of amplification and structuring of magnetic fields

Published online by Cambridge University Press:  18 July 2013

A. V. Getling ,
V. V. Kolmychkov  and
O. S. Mazhorova
A. V. Getling
Affiliation:
Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, Russia, email: A.Getling@mail.ru
V. V. Kolmychkov
Affiliation:
Keldysh Institute of Applied Mathematics, Moscow, Russia, email: ksv@keldysh.ru, olgamazhor@mail.ru
O. S. Mazhorova
Affiliation:
Keldysh Institute of Applied Mathematics, Moscow, Russia, email: ksv@keldysh.ru, olgamazhor@mail.ru
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Abstract

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Magnetoconvection in a horizontal layer of incompressible fluid is simulated numerically. The initial magnetic field is assumed to be uniform and horizontal. The interaction of quasi-ordered cellular convection with the magnetic field is shown to be able to produce bipolar (and also diverse more complex) configurations of a substantially amplified magnetic field. The operation of this mechanism, which can be regarded as a modification of the mechanism suggested by Tverskoi (1966), is controlled by the very topology of the cellular flow, should be manifest on various spatial scales, and does not require strong initial fields. Magnetic configurations develop both in the central parts of convection cells, where circulatory fluid motion “winds” magnetic field lines, and in the network formed by their peripheral regions due to the “sweeping” of magnetic field lines.

Keywords

Sun: magnetic fieldsconvection
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S294: Solar and Astrophysical Dynamos and Magnetic Activity , August 2012 , pp. 137 - 142
Copyright
Copyright © International Astronomical Union 2013 

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