  Pleione is a Be star that is in a 218 day orbit with a low-mass binary
companion. Recent numerical simulations have shown that a Be star disc can be
subject to breaking when material is actively being fed into the inner parts of
the disc. After breaking, the disc is composed of two rings: an inner ring that
is anchored to the stellar equator and an outer ring that is free to nodally
precess. A double ring disc may explain some of the observed variability in
Pleione. We model the nodal precession of the outer disc ring that is driven by
the companion on an observed timescale of $80.5\,\rm yr$. We find that the
outer ring of a broken disc in a binary with an eccentricity of $e_{\rm b}=
0.6$ can precess on the observed timescale and have an outer radius that is in
rough agreement with the observed disc size. An unbroken disc model cannot fit
both the observed precession rate and disc size. Suppression of Kozai-Lidov
driven disc eccentricity is more likely for a high binary eccentricity if the
disc extends to the tidal truncation radius.
