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

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Chromospheric Fine Structure

Part of the book series: International Astronomical Union/Union Astronomique Internationale ((IAUS,volume 56))

Abstract

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 flux from the deep convertion zone. As the flux rope rises throgh 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.

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Author information

Authors and Affiliations

  1. Max-Planck-Institut für Physik und Astrophysik, München, Germany

    F. Meyer & H. U. Schmidt

  2. Dept. of Applied Mathematics and Theoretical Physics, University of Cambridge, England

    N. O. Weiss

  3. Dept. of Applied Mathematics, University of Sydney, New South Wales, Australia

    P. R. Wilson

Authors
  1. F. Meyer
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  2. H. U. Schmidt
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  3. N. O. Weiss
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  4. P. R. Wilson
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Editor information

Editors and Affiliations

  1. High Altitude Observatory of the National Center for Atmospheric Research (Sponsored by the National Science Foundation), P.O. Box 3000, 80303, Boulder, Colo., USA

    R. Grant Athay

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© 1974 International Astronomical Union

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Meyer, F., Schmidt, H.U., Weiss, N.O., Wilson, P.R. (1974). A Theoretical Model for the Convection of Magnetic Flux in and near Sunspots. In: Athay, R.G. (eds) Chromospheric Fine Structure. International Astronomical Union/Union Astronomique Internationale, vol 56. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-2103-6_28

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  • DOI: https://doi.org/10.1007/978-94-010-2103-6_28

  • Publisher Name: Springer, Dordrecht

  • Print ISBN: 978-90-277-0288-3

  • Online ISBN: 978-94-010-2103-6

  • eBook Packages: Springer Book Archive

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