  SN2018ibb is a recently observed hydrogen poor super-luminous supernova which
appears to be powered by the decay of $30\;\rm{M_\odot}$ of radioactive nickel.
This supernova has been suggested to show hybrid signatures of a pair
instability supernova and an interacting supernova. In a previous paper, we
found that rotating, metal enriched pair instability supernova progenitors
appeared to check both of these boxes. In this paper, we model the lightcurves
of the pair instability supernovae using STELLA. We find that the STELLA models
can explain the overall shape of the bolometric lightcurve of SN2018ibb, though
not specific morphological features such as the luminosity peak or the bump at
roughly three hundred days after the peak. We also estimate the contribution
from interaction, and find that with relatively low wind velocities, the
circum-stellar medium originating from the stellar winds is consistent with the
evidence for interaction in the spectra. The observed values of the photosphere
velocity in the hundred days after peak luminosity are similar to the STELLA
models, but the deceleration is lower. This leads to the biggest inconsistency
which is the black body temperature of SN2018ibb being much hotter than any of
the STELLA models. We note that this high temperature (and the flat velocity)
may be difficult to reconcile with the long rise time of SN2018ibb, but
nevertheless conclude that if it is accurate, this discrepancy represents a
challenge for SN2018ibb being a robust PISN candidate. This result is
noteworthy given the lack of other scenarios for this supernova.
