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Hydrodynamical simulations of the solar dynamo

  • Part II Generation of Large-Scale Magnetic Fields
  • Conference paper
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Advances in Solar Physics

Part of the book series: Lecture Notes in Physics ((LNP,volume 432))

Abstract

Hydrodynamic simulations of the solar convection zone can be used to model the generation of differential rotation and magnetic fields, and to determine mean-field transport coefficients that are needed in mean-field models. The importance of the overshoot layer beneath the solar convection zone is discussed: it is the place where the magnetic field accumulates, although most of the field regeneration can still occur in the convection zone proper. We also discuss how systematically oriented bipolar regions can emerge from the convection zone where the magnetic field is highly intermittent.

The National Center for Atmospheric Research is sponsored by the National Science Foundation

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Authors and Affiliations

  1. HAO/NCAR, P.O. Box 3000, 80307-3000, Boulder, CO, USA

    Axel Brandenburg

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  1. Axel Brandenburg
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G. Belvedere M. Rodonò G. M. Simnett

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© 1994 Springer-Verlag

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Brandenburg, A. (1994). Hydrodynamical simulations of the solar dynamo. In: Belvedere, G., Rodonò, M., Simnett, G.M. (eds) Advances in Solar Physics. Lecture Notes in Physics, vol 432. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-58041-7_203

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  • DOI: https://doi.org/10.1007/3-540-58041-7_203

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  • Publisher Name: Springer, Berlin, Heidelberg

  • Print ISBN: 978-3-540-58041-6

  • Online ISBN: 978-3-540-48420-2

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