SN 1961V: A Pulsational Pair-Instability Supernova

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a $\sim 10^{40}$ erg s${}^{-1}$ star-like object could still be shining at the site of SN~1961V, but it has more likely been replaced by a massive accreting black hole.

arXiv comment18 pages, 11 figures, 3 tables; submitted to Astrophysical Journal, 5/9/22

References in corpus (40)

• GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs
• How Massive Single Stars End their Life
• Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions
• The Nucleosynthetic Signature of Population III
• Core-Collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars
• Pulsational Pair-Instability Supernovae
• Pulsational pair instability as an explanation for the most luminous supernovae
• On the role of continuum-driven eruptions in the evolution of very massive stars and Population III stars
• Mind the gap: The location of the lower edge of the pair instability supernovae black hole mass gap
• The Unprecedented 2012 Outburst of SN 2009ip: A Luminous Blue Variable Becomes a True Supernova
• Interacting Supernovae and Supernova Impostors. SN 2009ip, is this the end?
• Luminous Blue Variable eruptions and related transients: Diversity of progenitors and outburst properties
• Pair Instability Supernovae: Light Curves, Spectra, and Shock Breakout
• Discovery of Precursor LBV Outbursts in Two Recent Optical Transients: The Fitfully Variable Missing Links UGC 2773-OT and SN 2009ip
• Constraints from gravitational wave detections of binary black hole mergers on the ${}^{12}\mathrm{C}{\left(\alpha ,\gamma \right)}^{16}\mathrm{O}$ rate
• Setting the Stage for Circumstellar Interaction in Core-Collapse Supernovae II: Wave-Driven Mass Loss in Supernova Progenitors
• Type II-Plateau supernova radiation: dependencies on progenitor and explosion properties
• The Missing Luminous Blue Variables and the Bistability Jump
• The Pair-Instability Mass Gap for Black Holes
• Spectral Evolution of the Extraordinary Type IIn Supernova 2006gy
• Massive main sequence stars evolving at the Eddington limit
• Three Dimensional Radiation Hydrodynamic Simulations of Massive Star Envelopes
• The impact of stellar rotation on the black hole mass-gap from pair-instability supernovae
• Unmasking the Supernova Impostors
• Light-echoes from the plateau in Eta Carinae's Great Eruption reveal a two-stage shock-powered event
• Numerical Simulations of Convective 3-Dimensional Red Supergiant Envelopes
• Explosions Triggered by Violent Binary-Star Collisions: Application to Eta Carinae and other Eruptive Transients
• The Supernova Impostor Impostor SN 1961V: Spitzer Shows That Zwicky Was Right (Again)
• Magnetar-Powered Supernovae in Two Dimensions. I. Superluminous Supernovae
• Pulsational pair-instability supernovae: gravitational collapse, black-hole formation, and beyond
• The Low Detection Rate of Pair Instability Supernovae and the Effect of the Core Carbon Fraction
• It's Alive! The Supernova Impostor 1961V
• Pair-Instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves
• Evolutionary models of red supergiants: Evidence for a metallicity-dependent mixing length and implications for Type IIP supernova progenitors
• SN 2009ip after a decade: The luminous blue variable progenitor is now gone
• Massive Stellar Mergers as Precursors of Hydrogen-rich Pulsational Pair Instability Supernovae
• Possible Recovery of SN 1961V In Hubble Space Telescope Archival Images
• The Nature of SN 1961V
• Deep Late-Time Observations of the Supernova Impostors SN 1954J and SN 1961V

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