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Dynamics of the preflare magnetic field

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Abstract

Many theories of the solar flare process invoke storage of energy in the active region magnetic field above the solar photosphere. Observational evidence relating to such storage is rather unsatisfactory owing to our inability to observe the three-dimensional structure of the magnetic field. Indirect evidence comes from changes in structures presumed to trace the magnetic field, from changes in the line-of-sight and transverse components of the photospheric magnetic field, from mass flow patterns observed by proper motions and line-of-sight Doppler shifts, and from radio observations. These data tend to confirm that energy sufficient to produce flares can be stored in active region magnetic fields with a characteristic time scale of hours but critical observation are not yet available.

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Authors and Affiliations

  1. Kitt Peak National Observatory, 85726, Tucson, Ariz., USA

    John W. Harvey

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  1. John W. Harvey
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Operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.

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Harvey, J.W. Dynamics of the preflare magnetic field. Space Sci Rev 34, 55–62 (1983). https://doi.org/10.1007/BF00221196

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