Massive black holes are thought to populate the centres of most galaxies hosting spheroids. When these galaxies merge - a common occurrence in hierarchical cosmologies - they may give rise to long-lasting supermassive black hole binary (SBHB) systems. Stars that are not ejected from the nucleus during the merger can remain to form a nuclear disk or toroid, which can be used to infer information about the SBHB. In this talk, I will outline our attempts to model the stellar dynamics near a SBHB in order to characterize orbital stability and ejection mechanisms in these systems. As well, I will discuss the comparison of model stellar toroids to HST images of a suspected nuclear disk in a dwarf elliptical galaxy.