Illustration of the initial conditions. The color scale shows the logarithm of the density, the arrows show the velocity, and the solid white lines represent the magnetic field. From the polar axis (vertical axis) to the equatorial plane (horizontal axis), three different initial regions lie above the stellar photosphere and one region lies outside of the magnetosphere. The first region is an outflow from the star that emerges from the polar coronal hole. It is surrounded by the second region, in which the flow velocity has been reversed and the density enhanced to induce magnetospheric accretion. The second region starts on the equatorial plane from 0.03 AU to 0.09 AU. Inside this region lies a third region, corresponding to a dead or static zone without flow. It is located above the equatorial plane between the radius of the star at 0.011 AU and the inner disk radius 0.03 AU. The fourth region is the disk wind. It starts on the right of the last open field-line connected to the magnetosphere at ϖ(π/2) = 0.09 AU on the equatorial plane (solid white line) and extends above the accretion disk.