  I discuss the results of simplified three dimensional magnetohydrodynamic
simulations of the boundary layer between a disc and a non-rotating,
unmagnetized star. Strong magnetic fields, possibly approaching equipartition
with the thermal energy, occur in the boundary layer due to the shearing of
disc-generated fields. The mean boundary layer magnetic field, which is highly
variable on an orbital timescale, is estimated to exceed 50 kG for a CV with an
accretion rate of 10^(-9) solar masses per year. However, these fields do not
drive efficient angular momentum transport within the boundary layer. As a
consequence the radial velocity in the boundary layer is low, and the density
high.
