  Magnetohydrodynamic (MHD) simulations have been used to study disk accretion
to a rotating magnetized star with an aligned dipole moment. Quiescent initial
conditions were developed in order to avoid the fast initial evolution seen in
earlier studies. A set of simulations was performed for different stellar
magnetic moments and rotation rates. Simulations have shown that the disk
structure is significantly changed insidea radius r_{br} where magnetic braking
is significant. In this region the disk is strongly inhomogeneous. Radial
accretion of matter slows as it approaches the area of strong magnetic field
and a dense ring and funnel flow form at the magnetospheric radius r_m where
the magnetic pressure is equal to the total, kinetic plus thermal, pressure of
the matter.
