  In recent years, the viability of the pair-instability supernova (PISN)
scenario for explaining superluminous supernovae has all but disappeared except
for a few slowly-evolving examples. However, PISN are not predicted to be
superluminous throughout the bulk of their mass range. In fact, it is more
likely that the first PISN we see (if we have not seen one already) will not be
superluminous. Here, we present hydrodynamic simulations of PISNe for four
stellar models with unique envelope properties spanning the PISN mass range. In
addition, we compute synthetic light curves for comparison with current and
future observations. We also investigate, in the context of our most massive
model, the prospect of mixing in the supernova ejecta alleviating discrepancies
between current PISN models and the remaining superluminous candidate events.
To this end, we present the first published 3D hydrodynamic simulations of
PISNe. After achieving convergence between 1D, 2D, and 3D simulations we
examine mixing in the supernova ejecta and its affect on the bolometric light
curve. We observe slight deviations from spherical symmetry which increase with
the number of dimensions. We find no significant effects on the bolometric
light curve, however we conclude that mixing between the silicon and oxygen
rich layers caused by the Rayleigh-Taylor instability may affect spectra.
