  We investigate the properties of magnetized stars in the propeller regime
using axisymmetric numerical simulations. We modelled the propeller regime for
stars with realistically large magnetospheres (5-7 stellar radii), so that our
results could be applied to different types of magnetized stars, including
Classical T Tauri stars, cataclysmic variables, and accreting millisecond
pulsars. A wide range of propeller strengths has been studied, from very strong
propellers (where the magnetosphere rotates much more rapidly than the inner
disk) to very weak propellers (where the magnetosphere rotates only slightly
faster than the inner disc. In both propellers, matter is accumulated at the
inner disc for the majority of the time, while episodes of accretion onto the
star and ejection into the wind are relatively brief. The efficiency of the
propeller, which characterizes the part of inner disk matter flowing into the
wind, strongly depends on the fastness parameter omega_s: propeller efficiency
increases with omega_s. The properties of the winds are different in strong and
weak propellers. In the strong propellers, matter is accelerated rapidly above
the escape velocity and flows at a relatively small opening angle of 40-45
degrees. In the weak propellers, matter may flow faster or slower than the
escape velocity and at a large opening angle of 60-70 degrees. A star-disk
system loses energy and angular momentum. A part of the rotational energy of
the star is ejected to the magnetically-dominated (Poynting flux) jet, which is
only present in the strong propellers. The other part of the energy flows from
the inner disk into a propeller-driven wind. A star spins down partly due to
the flow of angular momentum from the star to the corona or to the Poynting
flux jet along the open field lines, and partly due to the flow of angular
momentum to the inner disk along the closed field lines.
