  Recent observations demonstrate that misalignments and other out-of-plane
structures are common in protoplanetary discs. Many of these have been linked
to a central host binary with an orbit that is inclined with respect to the
disc. We present simulations of misaligned circumbinary discs with a range of
parameters to gain a better understanding of the link between those parameters
and the disc morphology in the wave-like regime of warp propagation that is
appropriate to protoplanetary discs. The simulations confirm that disc tearing
is possible in protoplanetary discs as long as the mass ratio, $\mu$, and
disc-binary inclination angle, $i$, are not too small. For the simulations
presented here this corresponds to $\mu > 0.1$ and $i \gtrsim 40^\circ$. For
highly eccentric binaries, tearing can occur for discs with smaller
misalignment. Existing theoretical predictions provide an estimate of the
radial extent of the disc in which we can expect breaking to occur. However,
there does not seem to be a simple relationship between the disc properties and
the radius within the circumbinary disc at which the breaks appear, and
furthermore the radius at which the disc breaks can change as a function of
time in each case. We discuss the implications of our results for interpreting
observations and suggest some considerations for modelling misaligned discs in
the future.
