  We demonstrate the importance of general relativistic apsidal precession in
warped black hole accretion discs by comparing three - dimensional smoothed
particle hydrodynamic simulations in which this effect is first neglected, and
then included. If apsidal precession is neglected, we confirm the results of an
earlier magnetohydrodynamic simulation which made this assumption, showing that
at least in this case the $\alpha$ viscosity model produces very similar
results to those of simulations where angular momentum transport is due to the
magnetorotational instability. Including apsidal precession significantly
changes the predicted disc evolution. For moderately inclined discs thick
enough that tilt is transported by bending waves, we find a disc tilt which is
nonzero at the inner disc edge and oscillates with radius, consistent with
published analytic results. For larger inclinations we find disc breaking.
