Intensive optical photometry and linear polarimetry have detailed the morphology of a recent mass-loss episode of the Be star Omega Orionis. The continuum photometry and polarimetry were found to change in close concert. The H-alpha line photometry and polarimetry were also correlated, albeit to a lesser extent. The physical processes controlling the polarimetric and photometric changes are discussed, with limits being placed on both the time scale and the increase in envelope mass over the onset of this episode. It is suggested that this event can be traced to a marginal stellar instability.