Single-Fluid 2D Magnetohydrodynamic Simulation of Solar Wind Structure in Comparison to Ulysses Observations

Two dimensional Magnetohydrodynamic (MHD) equations with and without the momentum addi- tion respectively have been used to simulate the solar wind structure on the meridian plane. The results show that far away from the sun it isn’s solar magnetic field that induces the concave solar wind speed. Instead, there may be the fast speed streamer driven by the momentum addition and an interface between high and low speed streamers. The interaction between high and low speed streamers causes the sharp division.