SINGLE FLUID 2D MAGNETOHYDRODYNAMIC SIMULATION OF SOLAR WIND STRUCTURE

In this paper, single fluid 2D MagnetoHydroDynamic (MHD) equations with a momentum addition is used to simulate the solar wind structure on the meridian plane. With the comparison between the simulation results and observations by Ulysses, it is found that the form and deposited location of the momentum addition have great effect on solar wind velocity and density far away from the Sun. An appropriate momentum addition is adopted to calculate the solar wind velocity and density and obtained similar results with the Ulysses observations. It is found that the acceleration process simulated near the Sun agrees well with the data observed. The momentum addition should be deposited on 3.5-10 solar radii as a conclusion of the paper, and the result provides some clues for the problem of the solar wind acceleration mechanism.