  The evolution of an initially stellar dipole type magnetosphere interacting
with an accretion disk is investigated using numerical ideal MHD simulations.
The simulations follow several 1000 Keplerian periods of the inner disk. The
initial dipole type magnetic field develops into a spherically radial outflow
pattern with two main components both evolving into a quasi-stationary final
state. A neutral field line divides both components, along which small
plasmoids are ejected in irregular time intervals. The half opening angle of
the stellar wind cone varies from 30 to 55 degrees depending on the ratio of
the mass flow rates of disk wind and stellar wind. The maximum speed of the
outflow is about the Keplerian speed at the inner disk radius. An axial jet
forms during the first decades of rotation. However, this feature does not
survive on the very long time scale and a pressure driven low velocity flow
along the axis evolves.
