MHD Simulations of the Global Solar Corona and the Solar Wind
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.
KeywordsSolar Wind Coronal Hole Solar Eclipse Heliospheric Current Sheet Slow Solar Wind
- Crooker NU, Gosling JT, Kahler SW (2002a) Reducing heliospheric magnetic flux from coronal mass ejections without disconnection. J Geophys Res (Space Phys) 107:3–1Google Scholar
- Lundquist LL, Fisher GH, McTiernan JM, Régnier S (2004) In: Walsh RW, Ireland J, Danesy D, Fleck B (eds) Using synthetic emission images to constrain heating parameters. ESA SP-575: SOHO 15 coronal heating. ESA, Noordwijk, pp 306–Google Scholar
- Mikić Z, Linker JA (1996) The large-scale structure of the solar corona and inner heliosphere. In: Winterhalter D, Gosling JT, Habbal SR, Kurth WS, Neugebauer M (eds) Solarwind eight, Proceedings of the eighth international solarwind conference, American Institute of Physics conference proceedings 382. American Institute of Physics, Woodbury, New York, 1996, pp 104–107Google Scholar
- Usmanov AV (1995) A global 3-DMHD model of the solar wind with Alfven waves. In: Solar wind conference, pp 65–+Google Scholar