  A general model of magnetically controlled accretion onto T Tauri stars is
presented. In this model the magnetic field is oriented arbitrarily in relation
to the star's rotation axis. The resultant interplay between the magnetic field
and accretion disc causes a variable accretion rate. The dominant timescale of
this variability is the beat frequency between the stellar rotation frequency
and the orbital frequency at the magnetosphere boundary. This model is
analogous to that developed to explain quasi-periodic oscillations in low-mass
X-ray binaries.
