Physics of superluminous supernovae

Abstract

Understanding how massive stars die as supernovae (SNe) is a crucial question in modern astrophysics. SNe are powerful stellar explosions and key drivers in the cosmic baryonic cycles by injecting their explosion energy and heavy elements to the interstellar medium that forms new stars. After decades of effort, astrophysicists have built up a stand model for the explosion mechanism of massive stars. However, this model is challenged by new kinds of stellar explosions discovered in the recent transit surveys. In particular, the new population called superluminous SNe, which are a hundred times brighter than typical SNe, is revolutionizing our understanding of SNe. New studies suggest the superluminous SNe are associated with the unusual demise of very massive stars and their extreme SNe powered by the radioactive isotopes or compact objects formed after the explosion. Studying these SNe fills a gap of knowledge between the death of massive stars and their explosions; furthermore, we may apply their intense luminosity to light up the distant universe. This paper aims to provide a timely review of superluminous SNe physics, focusing on the latest development of their theoretical models.