  We present the results of axisymmetric simulations of MRI-driven accretion
onto a rapidly rotating, magnetized star accreting in the propeller regime. The
stellar magnetosphere corotates with the star, forming a centrifugal barrier at
the disc-magnetosphere boundary which inhibits matter accretion onto the star.
Instead, the disc matter accumulates at the disc-magnetosphere interface and
slowly diffuses into the inner magnetosphere where it picks up angular momentum
and is quickly ejected from the system as an outflow. Due to the interaction of
the matter with the magnetosphere, this wind is discontinuous and is launched
as discrete plasmoids. If the ejection rate is lower than the disc accretion
rate, the matter accumulates at the disc-magnetosphere boundary faster than it
can be ejected. In this case, accretion onto the star proceeds through the
episodic accretion instability in which episodes of matter accumulation are
followed by simultaneous accretion and ejection. During the accretion phase of
this instability in which matter flows onto the star in funnel streams, we
observe a corresponding rise in the outflow rate. Both the accretion and
ejection processes observed in our simulations are highly non-stationary. The
stars undergo strong spin-down due to the coupling of the stellar field with
the disc and corona and we measure the spin-down timescales of around 1 Myr for
a typical CTTS in the propeller regime.
