Superluminous supernovae (SLSNe) are a population of supernovae (SNe) whose peak luminosities are much larger than those of canonical SNe. Although SLSNe were simply defined by their peak luminosity at first, it is currently recognized that they show rich spectroscopic diversities including hydrogen-poor (Type I) and hydrogen-rich (Type II) subtypes. The exact mechanisms making SLSNe luminous are still not fully understood, but there are mainly four major suggested luminosity sources (radioactive decay of 56Ni, circumstellar interaction, magnetar spin-down, and fallback accretion). We provide an overview of observational properties of SLSNe and major theoretical models for them. Future transient surveys are expected to discover SLSNe at high redshifts which will provide a critical information in revealing their nature.
@article{arxiv.2407.12302,
title = {Superluminous supernovae},
author = {Takashi J. Moriya},
journal= {arXiv preprint arXiv:2407.12302},
year = {2024}
}
Comments
This is a pre-print of a chapter for the Encyclopedia of Astrophysics (edited by I. Mandel, section editor F.R.N. Schneider) to be published by Elsevier as a Reference Module