With an increasing number of superluminous supernovae ( SLSNe ) discovered the question of their origin remains open and causes heated debates in the supernova 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 material ejected before the explosion .
Based on current observations of SLSNe , the PISN origin has been disfavoured for a number of reasons .
Many PISN models provide overly broad light curves and too reddened spectra , because of massive ejecta and a high amount of nickel .
In the current study we re-examine PISN properties using progenitor models computed with the GENEC code .
We calculate supernova explosions with FLASH and light curve evolution with the radiation hydrodynamics code STELLA .
We find that high-mass models ( 200 \mathrm { M } \odot and 250 \mathrm { M } \odot ) at relatively high metallicity ( Z = 0.001 ) do not retain hydrogen in the outer layers and produce relatively fast evolving PISNe Type I and might be suitable to explain some SLSNe .
We also investigate uncertainties in light curve modelling due to codes , opacities , the nickel-bubble effect and progenitor structure and composition .