Surface Driven Evolution and Activity of Atmospheric Magnetic Structures

  • G. van Hoven
  • Y. Mok
  • D. L. Hendrix
  • Z. Mikić

Abstract

The magnetic structure of the solar corona influences solar activity, including coronal heating and solar flares. Magnetic loops and arcades are observed to dominate the structure of the corona; they are formed by the interaction of high-β photospheric convection with low-β coronal magnetic fields. We show the results of 3-D MHD simulations of the response of coronal fields to convective and shear-flow driving from the photosphere. The principal examples include the micro-flare activity in the Parker loop-heating archetype (Schnack and Mikić 1994), and the formation and revolution of 3-D coronal loops (Van Hoven et al. 1995a).

Keywords

Magnetic Reconnection Solar Corona Coronal Loop Magnetic Loop Coronal Heating 
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 1996

Authors and Affiliations

  • G. van Hoven
    • 1
  • Y. Mok
    • 1
  • D. L. Hendrix
    • 1
  • Z. Mikić
    • 2
  1. 1.Department of Physics and AstronomyUniversity of CaliforniaIrvineUSA
  2. 2.Science Applications International CorporationSan DiegoUSA

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