Abstract
For the initial mass range 140<M<260 M⊙, stars die in a thermonuclear runaway triggered by the pair‐production instability. Their supernovae can be remarkably energetic and synthesize considerable amounts of radioactive isotopes. We present a set of calculations modeling the evolution, explosion, and observational signatures of pair‐instability supernovae spanning a range of initial masses and envelope structures. We compare the resulting light curves and spectra to recent observations of luminous nearby supernovae, including the most compelling candidate pair‐instability event to date, SN2007bi.
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