HR: 0830h
AN: SH21B-0138    [PDF]
TI: Three-Dimensional MHD Modeling of the Solar Corona and Solar Wind
AU: Goldstein, M L
EM: melvyn.l.goldstein@nasa.gov
AF: NASA Goddard Space Flight Center, Code 692, Greenbelt, MD 20771 United States
AU: * Usmanov, A V
EM: arcadi.usmanov@gsfc.nasa.gov
AF: NASA Goddard Space Flight Center, Code 692, Greenbelt, MD 20771 United States
AB: 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 Alfv\'en 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.
DE: 2102 Corotating streams
DE: 2134 Interplanetary magnetic fields
DE: 2169 Sources of the solar wind
DE: 7509 Corona
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting