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Magnetohydrodynamic theories of solar flares

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Abstract

Our current understanding of the MHD of the flare process is summarised, with some emphasis on processes which produce strong impulsive electric fields and current filamentation. As an introduction, a description of the two main types of flare (i.e., simple-loop and two-ribbon) is given, together with an account of the two branches of reconnection theory (tearing modes and the Petschek-Sonnerup mechanism). Modern numerical experiments of reconnection suggest impulsive bursty acceleration of particles in many small regions of width a hundred kilometres or less. This is followed by a discussion of the eruptive instability thought to initiate a large flare and of the reconnection process of energy release. Finally, the role of emerging flux and horizontally moving satellite sunspots is discussed briefly.

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Authors and Affiliations

  1. Applied Mathematics Department, St. Andrews University, KY16 9SS, Scotland

    E. R. Priest

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  1. E. R. Priest
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Proceedings of the Workshop on Radio Continua during Solar Flares, held at Duino (Trieste), Italy, 27–31 May, 1985.

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Priest, E.R. Magnetohydrodynamic theories of solar flares. Sol Phys 104, 1–18 (1986). https://doi.org/10.1007/BF00159941

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