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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
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
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