Articles | Volume 17, issue 5
Ann. Geophys., 17, 578–582, 1999

Special issue: Solar System Plasmas

Ann. Geophys., 17, 578–582, 1999

  31 May 1999

31 May 1999

Simulating solar MHD

M. Schüssler M. Schüssler
  • Kiepenheuer-Institut für Sonnenphysik (KIS) Schöneckstr. 6, D-79104 Freiburg, Germany
  • e-mail:

Abstract. Two aspects of solar MHD are discussed in relation to the work of the MHD simulation group at KIS. Photospheric magneto-convection, the nonlinear interaction of magnetic field and convection in a strongly stratified, radiating fluid, is a key process of general astrophysical relevance. Comprehensive numerical simulations including radiative transfer have significantly improved our understanding of the processes and have become an important tool for the interpretation of observational data. Examples of field intensification in the solar photosphere ('convective collapse') are shown. The second line of research is concerned with the dynamics of flux tubes in the convection zone, which has far-reaching implications for our understanding of the solar dynamo. Simulations indicate that the field strength in the region where the flux is stored before erupting to form sunspot groups is of the order of 105 G, an order of magnitude larger than previous estimates based on equipartition with the kinetic energy of convective flows.

Key words. Solar physics · astrophysics and astronomy (photosphere and chromosphere; stellar interiors and dynamo theory; numerical simulation studies).

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