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Magnetic Reconnection Models of Flares

  • T. G. Forbes
Part of the Astrophysics and Space Science Library book series (ASSL, volume 143)

Abstract

The most feasible energy source for solar and stellar flares is the energy stored in coronal magnetic fields. To convert a significant fraction of this energy into heat and kinetic energy in a short time requires rapid change in the topology of the magnetic fields, and hence, rapid reconnection of field lines. Recent numerical and analytical models of solar flares suggest that the magnetic energy released by reconnection drives chromospheric ablation in the flare ribbons. Simple theoretical arguments based on compressible reconnection theory predict that the temperature of the ablated plasma should be about 1.03 × 106 B0.62 oK where B is the coronal magnetic field strength in Gauss.

Keywords

Field Line Current Sheet Solar Flare Magnetic Reconnection Coronal Magnetic Field 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Kluwer Academic Publishers 1988

Authors and Affiliations

  • T. G. Forbes
    • 1
  1. 1.Institute for the Study of Earth, Oceans and SpaceUniversity of New HampshireDurhamUSA

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