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 .