A. V. Usmanov, M. L. Goldstein, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
We
present a fully three-dimensional steady-state MHD model of the solar corona
and solar wind that includes the momentum and energy addition from Alfvén
waves propagating away from the Sun. The WKB approach is employed to
statistically describe the effect of Alfvén waves on the background flow and
vice versa. This approximation is appropriate for the waves with
wavelengths shorter than local characteristic scales and does not require a
high resolution description of the momentum and energy transformation
between the waves and the flow. We compare output from the model with
Ulysses observations and show that the wave-drive model reproduces the
bimodal structure of the solar wind observed by Ulysses.