  We present results of global three-dimensional (3D) magnetohydrodynamic (MHD)
simulations of accretion onto magnetized stars where both the magnetic and
rotational axes of the star are tilted about the rotational axis of the disc.
We observed that initially the inner parts of the disc are warped, tilted, and
process due to the magnetic interaction between the magnetosphere and the disc.
Later, larger tilted discs form with the size increasing with the magnetic
moment of the star. The normal vector to the discs are tilted at different
angles, from 5-10 degrees up to 30-40 degrees. Small tilts may result from the
winding of the magnetic field lines about the rotational axis of the star and
the action of the magnetic force which tends to align the disc. Another
possible explanation is the magnetic Bardeen-Petterson effect in which the disc
settles in the equatorial plane of the star due to precessional and viscous
torques in the disc. Tilted discs slowly precess with the time scale of the
order of 50 Keplerian periods at the reference radius (approx. 3 stellar
radii). Our results can be applied to different types of stars where signs of
tilted discs and/or slow precession have been observed.
