A global MHD solar wind model with WKB Alfven waves: Comparison with Ulysses data

We use a steady state global axisymmetric MHD model to reproduce quantitati vely the Ulysses observations during its first fast latitude traversal in 1 994-1995. In particular, we are able to account for the transformation of a surface dipole magnetic field near the Sun into the configuration observed at large heliocentric distances. The MHD equations are solved by combining a time relaxation numerical technique with a marching-along-radius method. We assume that Alfven waves, propagating outward from the Sun, provide add itional heating and acceleration to the flow. Only solutions with waves rep roduce the plasma parameters observed in title high-latitude fast solar win d. We show that the meridional distribution of solar wind plasma and magnet ic field parameters is dominated by two processes. First, inside similar to 24 R-circle dot both the plasma velocity and magnetic field relax toward a latitude-independent profile outside the equatorial current sheet (where m agnetic forces dominate over thermal and wave gradient forces). Second, out side similar to 24 R-circle dot there is another meridional redistribution due to a poleward thermal pressure gradient that produces a slight poleward gradient in the radial velocity and an equatorward gradient in the radial component of the magnetic field. We reproduce the observed bimodal structur e and morphology of both fast and slow wind and Show that computed paramete rs are generally in agreement with both in situ data and conditions inferre d to be characteristic of the solar corona.