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A Theoretical Model for the Convection of Magnetic Flux in and near Sunspots

Published online by Cambridge University Press:  14 August 2015

F. Meyer ,
H. U. Schmidt ,
N. O. Weiss  and
P. R. Wilson
F. Meyer
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, München, Germany
H. U. Schmidt
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, München, Germany
N. O. Weiss
Affiliation:
Dept. of Applied Mathematics and Theoretical Physics, University of Cambridge, England
P. R. Wilson
Affiliation:
Dept. of Applied Mathematics, University of Sydney, New South Wales, Australia

Abstract

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In this paper we investigate the physical processes that lead to the growth and decay of magnetic flux in and near sunspots.

An initial phase of rapid growth is characterized by the emergence of magnetic flux from the deep convection zone. As the flux rope rises through the surface the magnetic field is swept to the junctions of the supergranular network where sunspots are formed. These flux concentrations follow the footpoints of the emergent flux rope as they rapidly move apart.

Type
Part VI: Evolution of Chromospheric Fine Structures
Information
Symposium - International Astronomical Union , Volume 56: Chromospheric Fine Structure , 1974 , pp. 235 - 237
Copyright
Copyright © Reidel 1974