SN 1961V: A Pulsational Pair-Instability Supernova

TL;DR

This paper models SN 1961V as a pulsational pair-instability supernova, successfully reproducing its light curve and exploring different progenitor scenarios with implications for black hole remnants.

Contribution

It introduces detailed PPISN models for SN 1961V, considering various subclasses and carbon abundances, providing insights into its progenitor and explosion characteristics.

Findings

Models reproduce the observed light curve of SN 1961V.

Progenitor mass estimates range from 100 to 115 solar masses.

Black hole remnants of 40 to 45 solar masses are predicted.

Abstract

We explore a variety of models in which SN~1961V, one of the most enigmatic supernovae (SNe) ever observed, was a pulsational pair-instability supernova (PPISN). Successful models reproduce the bolometric light curve of the principal outburst and, in some cases, the emission one year before and several years afterward. All models have helium-rich ejecta, bulk hydrogenic velocities near 2000 km s$^{-1}$, and total kinetic energies from 4 to 8 $\times 10^{50}$ erg. Each eventually leaves behind a black hole remnant. Three subclasses of PPISN models are explored, each with two different choices of carbon abundance following helium burning. Carbon is an important parameter because shell carbon burning can weaken the explosion. The three subclasses correspond to situations where SN~1961V and its immediate afterglow were: a) a single event; b) the first of two or more pulsational events separated by decades or centuries; or c) the latter stages of a complex explosion that had already been going on for a year or more. For the low carbon case, the main sequence mass for SN~1961V's progenitor would have been 100 to 115 \Msun; its pre-SN helium core mass was 45 to 52 \Msun; and the final black hole mass, 40 to 45 \Msun. For the high-carbon case, these values are increased by roughly 20 to 25\%. In some PPISN models, a $\sim10^{40}$ erg s$^{-1}$ star-like object could still be shining at the site of SN~1961V, but it has more likely been replaced by a massive accreting black hole.