Top left: a pure stellar dipole field extends into the disk with a vertical field near the equator. Top right: the existence of a stellar wind stretches the magnetic field and opens it up at the Alfvén point. Thus, the field near/inside the disk is expected to be radial, not vertical. If it is affected by the disk rotation, it is azimuthal, but still not vertical. Bottom: if the stellar dipole field is tilted, the field is still mostly radial.