Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...595l..57r&link_type=abstract
The Astrophysical Journal, Volume 595, Issue 1, pp. L57-L61.
Astronomy and Astrophysics
Astronomy
89
Interplanetary Medium, Methods: Numerical, Magnetohydrodynamics: Mhd, Sun: Solar Wind, Sun: Evolution, Sun: Magnetic Fields
Scientific paper
We present a new compressible MHD model for simulating the three-dimensional structure of the solar wind under steady state conditions. The initial potential magnetic field is reconstructed throughout the computational volume using the source surface method, in which the necessary boundary conditions for the field are provided by solar magnetogram data. The solar wind in our simulations is powered by the energy interchange between the plasma and large-scale MHD turbulence, assuming that the additional energy is stored in the ``turbulent'' internal degrees of freedom. In order to reproduce the observed bimodal structure of the solar wind, the thermodynamic quantities for the initial state are varied with the heliographic latitude and longitude depending on the strength of the radial magnetic field.
DeZeeuw Darren L.
Gombosi Tamas I.
Liewer Paulett
Luhmann Janet
Manchester Ward IV
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