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Formation of intense magnetic fields near the surface of the Sun

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Abstract

Convection concentrates magnetic flux into ropes between granules in the solar photosphere, with average fields of up to 1500 G. The magnetic energy density is locally much greater than the kinetic energy density. Theoretical limits to the amplification of magnetic fields by convection are analysed and related to the observations.

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Authors and Affiliations

  1. Astronomy Centre, University of Sussex, Falmer, Brighton, UK

    D. J. Galloway

  2. Department of Mathematics, Massachusetts Institute of Technology, Cambridge, Massachusetts, 02139

    M. R. E. Proctor

  3. Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Silver Street, Cambridge, UK

    N. O. Weiss

Authors
  1. D. J. Galloway
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  2. M. R. E. Proctor
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  3. N. O. Weiss
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Galloway, D., Proctor, M. & Weiss, N. Formation of intense magnetic fields near the surface of the Sun. Nature 266, 686–689 (1977). https://doi.org/10.1038/266686a0

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  • DOI: https://doi.org/10.1038/266686a0

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