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We build on our previous work involving smoothed particle hydrodynamicsimulations of Be stars, by using the model that exhibited disc tearing asinput into the three-dimensional Monte Carlo radiative transfer code HDUST topredict observables from a variety of viewing angles throughout the disctearing process. We run one simulation at the start of each orbital period from20 to 72 orbital periods, which covers two complete disc tearing events. Theresulting trends in observables are found to be dependent on the relativeposition of the observer and the tearing disc. The $\rm H\alpha$ equivalentwidth, $V$ magnitude, and polarization can all increase or decrease in anycombination depending on the viewpoint of the observer. The $\rm H\alpha$ lineprofile also displays changes in strength and peak separation throughout thetearing process. We show how the outer disc of the torn system can have a largeeffect on the $\rm H\alpha$ line profile, and also contributes to awavelength-dependent polarization position angle, resulting in a similarsawtooth shape to the polarization percentage. Finally, we compare ourpredictions to Pleione (28 Tau) where evidence has suggested that a disctearing event has occurred in the past. We find that our tearing disc model canbroadly match the trends seen in Pleione's observables, as well as produce thetwo-component $\rm H\alpha$ lines observed in Pleione. This is the strongestevidence, thus far, of Pleione's disc having indeed experienced a tearingevent.

Disc Tearing in a Be Star: Predicted 3D Observations