  We observed persistent high-frequency oscillations of the boundary layer near
an accreting, weakly-magnetized star in global 3D MHD simulations. The tilted
dipole magnetic field is not strong enough to open a gap between the star and
the disk. Instead, it forms a highly-wrapped azimuthal field near the surface
of the star which slows down rotation of the disk matter, while a small tilt of
the field excites oscillations of the boundary layer with a frequency below the
Keplerian frequency. This mechanism may be responsible for the high-frequency
oscillations in accreting neutron stars, white dwarfs and classical T Tauri
stars.
