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Solar Physics

, Volume 50, Issue 1, pp 85–98 | Cite as

Magnetic reconnection in the corona and the loop prominence phenomenon

  • R. A. Kopp
  • G. W. Pneuman
Article

Abstract

Many classes of transient solar phenomena, such as flares, flare sprays, and eruptive prominences, cause major disruptions in the magnetic geometry of the overlying corona. Typically, the results from Skylab indicate that pre-existing closed magnetic loops in the corona are torn open by the force of the disruption. We examine here some of the theoretical consequences to be expected during the extended relaxation phase which must follow such events. This phase is characterized by a gradual reconnection of the outward-distended field lines. In particular, the enhanced coronal expansion which occurs on open field lines just before they reconnect appears adequate to supply the large downward mass fluxes observed in Ha loop prominence systems that form during the post-transient relaxation. In addition, this enhanced flow may produce nonrecurrent high speed streams in the solar wind after such events. Calculations of the relaxation phase for representative field geometries and the resulting flow configurations are described.

Keywords

Flare Solar Wind Magnetic Reconnection Relaxation Phase High Speed Stream 
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

© D. Reidel Publishing Company 1976

Authors and Affiliations

  • R. A. Kopp
    • 1
  • G. W. Pneuman
    • 1
  1. 1.High Altitude Observatory, National Center for Atmospheric ResearchBoulderU.S.A.

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