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Superluminous supernovae
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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.
Forward citations
Cited by 2 Pith papers
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AT2019ijn: a fast-rising, slow-decaying blue optical transient with exceptionally bright radio emission
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Insights from Modeling Magnetar-driven Light Curves of Stripped-envelope Supernovae
A unified magnetar spin-down model reproduces the bolometric light curves of 11 stripped-envelope supernovae, but several reported correlations follow from the fitting formulas rather than from independent physics.
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