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Thermal evolution of current sheets and flash phase of solar flares

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Abstract

The physical conditions in a stationary flow of the Petchek type, allowing reconnection between flux emerging from below the solar photosphere and a preexisting magnetic field, are discussed. It is shown that, when rising in the solar atmosphere, the reconnection region has at first a rather low temperature as compared with its environment. Above a certain critical height, however, this low temperature thermal equilibrium often ceases to be possible, and the sheet rapidly heats, seeking a new thermal equilibrium. During this dynamical process, current-driven microinstabilities may be triggered in the current sheet, giving rise to an enhanced resistivity. High energy particles might be produced by the induced electric field developed during the rapid readjustment of MHD flows that results from this change in the transport properties of the plasma.

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Authors and Affiliations

  1. Observatoire de Meudon, France

    J. Heyvaerts

  2. University of St. Andrews, Scotland

    E. R. Priest

Authors
  1. J. Heyvaerts
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  2. E. R. Priest
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Heyvaerts, J., Priest, E.R. Thermal evolution of current sheets and flash phase of solar flares. Sol Phys 47, 223–231 (1976). https://doi.org/10.1007/BF00152260

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  • DOI: https://doi.org/10.1007/BF00152260

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