  We investigate spherical accretion to a rotating magnetized star in the
"propeller" regime using axisymmetric resistive magnetohydrodynamic
simulations. The regime is predicted to occur if the magnetospheric radius is
larger than the corotation radius and smaller than the light cylinder radius.
The simulations show that accreting matter is expelled from the equatorial
region of the magnetosphere and that it moves away from the star in a
supersonic, disk-shaped outflow. At larger radial distances the outflow slows
down and becomes subsonic. The equatorial matter outflow is initially driven by
the centrifugal force, but at larger distances the pressure gradient force
becomes significant. We find the fraction of the Bondi accretion rate which
accretes to the surface of the star.
