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Flux Separation in Photospheric Magnetoconvection

Published online by Cambridge University Press:  13 May 2016

N. O. Weiss  and
M. R. E. Proctor
N. O. Weiss
Affiliation:
Dept. of Applied Mathematics and Theoretcal Physics, University of Cambridge, Cambridge CB3 9EW, UK
M. R. E. Proctor
Affiliation:
Dept. of Applied Mathematics and Theoretcal Physics, University of Cambridge, Cambridge CB3 9EW, UK

Abstract

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Numerical experiments on three-dimensional magnetoconvection in a stratified compressible layer reveal a range of different patterns, depending on the strength of the imposed magnetic field. As the field is decreased there is a transition from small-scale plumes, in the magnetically dominated regime, to large-scale vigorous plumes when the field is dominated by the motion. In the intermediate regime magnetic flux separates from the motion, so that there are almost field-free regions, with clusters of vigorous plumes, surrounded by regions where the Lorentz force is strong enough to control the dynamics. There is a range of field strengths where either small-scale plumes or flux-separated solutions can persist, depending on initial conditions for the computation. These results can be related to magnetic features at the surface of the Sun.

Type
Session II: Convection Zone and Local Area Helioseismology
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 219 - 221
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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