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Twists and rotations of solar magnetic fields

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Abstract

Evidence is reviewed and extended that most, if not all, solar magnetic fields emerge as highly concentrated (⪞4000 gauss)helically twisted flux ropes, made up of hundreds or thousands of individually twisted flux fibers. The pitch angles of the twists are estimated as ⪝10° in the submerged flux ropes and roughly 1° in the flux fibers, but increase by large factors during and following emergence. The upward transmission of magnetic stresses and motions from the submerged flux-rope sections are major factors in solar physics. The helical twists account for the creation of sunspots and for their stability, fine structure, and mode of decay. They are basic features of the atmospheric structures, from the largest prominences and flare events down to arch filament systems and the smallest network components.

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Authors and Affiliations

  1. Division of Applied Physics, CSIRO, Sydney, Australia

    J. H. Piddington (Visiting Astronomer, Kitt Peak National Observatory (operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation)

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  1. J. H. Piddington
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Piddington, J.H. Twists and rotations of solar magnetic fields. Astrophys Space Sci 75, 273–287 (1981). https://doi.org/10.1007/BF00648642

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  • DOI: https://doi.org/10.1007/BF00648642

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