A magnetohydrodynamic simulation of the single-fluid 2-D structure of the solar wind

The system of single-fluid 2-D magnetohydrodynamic (MHD) equations incorporating the momentum term is simulated and the structure of the solar wind in the meridian plane is acquired. The form and location of the momentum addition have an important effect on the velocity and proton density of the solar wind in distant places. By locating the addition in an appropriate region (between 3.5 and 10 solar radii), we got results on the velocity and proton density agreeing with the Ulysses observations.