  Since the emergence of the new class of extremely bright transients,
super-luminous supernovae (SLSNe), three main mechanisms to power their light
curves (LCs) have been discussed. They are the spin-down of a magnetar,
interaction with circumstellar material, and the decay of large amounts of
radioactive nickel in pair-instability supernovae (PISNe). Given the high
degree of diversity seen within the class, it is possible that all three
mechanisms are at work. PISN models can be self- consistently simulated from
the main sequence phase of very massive stars (VMS) through to their explosion.
These models robustly predict large amounts of radioactive nickel and thus very
luminous SN events. However, PISN model LCs evolve more slowly than even the
slowest evolving SLSNe. Multidimensional effects on the ejecta structure,
specifically the mixing of radioactive nickel out to large radii, could
alleviate this discrepancy with observation. Here we explore the
multidimensional effects on the LC evolution by simulating the explosion phase
in 1D, 2D, and 3D. We find that the ejecta from the multidimensional
simulations have slightly shallower abundance gradients due to mixing at shell
boundaries. We compute synthetic LCs whose shapes show no discernible
differences due to the multidimensional effects.
