Surface Driven Evolution and Activity of Atmospheric Magnetic Structures

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


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).


Magnetic Reconnection Solar Corona Coronal Loop Magnetic Loop Coronal Heating 
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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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