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With an increasing number of superluminous supernovae (SLSNe) discovered thequestion of their origin remains open and causes heated debates in thesupernova community. Currently, there are three proposed mechanisms for SLSNe:(1) pair-instability supernovae (PISN), (2) magnetar-driven supernovae, and (3)models in which the supernova ejecta interacts with a circumstellar materialejected before the explosion. Based on current observations of SLSNe, the PISNorigin has been disfavoured for a number of reasons. Many PISN models provideoverly broad light curves and too reddened spectra, because of massive ejectaand a high amount of nickel. In the current study we re-examine PISN propertiesusing progenitor models computed with the GENEC code. We calculate supernovaexplosions with FLASH and light curve evolution with the radiationhydrodynamics code STELLA. We find that high-mass models (200 and 250 solarmasses) at relatively high metallicity (Z=0.001) do not retain hydrogen in theouter layers and produce relatively fast evolving PISNe Type I and might besuitable to explain some SLSNe. We also investigate uncertainties in lightcurve modelling due to codes, opacities, the nickel-bubble effect andprogenitor structure and composition.

Fast evolving pair-instability supernova models: evolution, explosion, light curves