2D MHD Models of the Large Scale Solar Corona

Details 2D MHD Models of the Large Scale Solar Corona 2D MHD Models of the Large Scale Solar Corona

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..331e&link_type=abstract

SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 331-3

Other

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Interplanetary Magnetic Fields

Scientific paper

By solving the equations of ideal MHD the interaction of an isothermal coronal plasma with a dipole-like magnetic field is studied. We vary the coronal temperature and the magnetic field strength to investigate how the plasma and the magnetic field interact to determine the structure of the large scale solar corona. When our numerical calculations are initiated with an isothermal solar wind in a dipole magnetic field, the equations may be integrated to a steady state. Open and closed regions are formed. In the open regions the atmosphere expands into a super-sonic wind, and in the closed regions the plasma is in hydrostatic equilibrium. We find that the magnetic field configuration in the outer corona is largely determined by the equatorial current sheet.

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