MHD Simulations of the Global Solar Corona and the Solar Wind

  • Roberto Lionello
  • Jon A. Linker
  • Zoran Mikić
  • Pete Riley
  • Viacheslav S. Titov
Chapter
Part of the IAGA Special Sopron Book Series book series (IAGA, volume 4)

Abstract

We describe the latest applications of our global three-dimensional magnetohydrodynamic (MHD) model of the solar corona and the solar wind. The model uses boundary conditions based on observed photospheric magnetic fields. It has been used in the simplified, “polytropic” approximation of the energy equation to study the geometrical and topological properties of the magnetic field (e.g., the location and evolution of corona holes, the reproduction of streamer structure, the location of the heliospheric current sheet). However, this approximation does not reproduce the density and temperature contrasts between open and closed-field regions and does not address data from EUV and X-ray emission. Our improved MHD model that includes energy transport (radiative losses, anisotropic thermal conduction, and coronal heating) in the transition region and solar corona is capable of reproducing many emission properties as observed by SoHO and Hinode.

Keywords

Solar Wind Coronal Hole Solar Eclipse Heliospheric Current Sheet Slow Solar Wind 
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

© Springer Science+Business Media B.V. 2011

Authors and Affiliations

  • Roberto Lionello
    • 1
  • Jon A. Linker
    • 1
  • Zoran Mikić
    • 1
  • Pete Riley
    • 1
  • Viacheslav S. Titov
    • 1
  1. 1.Predictive Science, Inc.San DiegoUSA

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