  Observational evidence suggests that some very massive stars in the local
Universe may die as pair-instability supernovae. We present 2D simulations of
the pair-instability supernova of a non-zero metallicity star. We find that
very little mixing occurs in this explosion because metals in the stellar
envelope drive strong winds that strip the hydrogen envelope from the star
prior to death. Consequently, a reverse shock cannot form and trigger fluid
instabilities during the supernova. Only weak mixing driven by nuclear burning
occurs in the earliest stages of the supernova, and it is too weak to affect
the observational signatures of the explosion.
