Three-Dimensional MHD Modeling of the Solar Corona and Solar Wind

Details Three-Dimensional MHD Modeling of the Solar Corona and Solar Wind Three-Dimensional MHD Modeling of the Solar Corona and Solar Wind

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh21b0138g&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH21B-0138

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2102 Corotating Streams, 2134 Interplanetary Magnetic Fields, 2169 Sources Of The Solar Wind, 7509 Corona

Scientific paper

We present simulation results from a fully three-dimensional MHD solar wind model with a tilted-dipole magnetic field on the Sun, resembling conditions near solar activity minimum. The polytropic single-fluid MHD equations, which incorporate Alfvén wave momentum and energy addition in the WKB approximation, are solved in the corotating frame by a combination of time-relaxation and marching-along-radius methods. Boundary conditions are prescribed at the coronal base and the computational region extends out to 1 AU. We show that simulation results are in agreement with the latitudinal profiles observed by Ulysses during its first fast south-to-north transition in 1994-1995.

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