Pulsational Pair-Instability Supernovae

  title={Pulsational Pair-Instability Supernovae},
  author={S. E. Woosley},
  journal={arXiv: High Energy Astrophysical Phenomena},
  • S. Woosley
  • Published 31 August 2016
  • Physics
  • arXiv: High Energy Astrophysical Phenomena
The final evolution of stars in the mass range 70 - 140 solar masses is explored. Depending upon their mass loss history and rotation rates, these stars will end their lives as pulsational pair-instability supernovae producing a great variety of observational transients with total durations ranging from weeks to millennia and luminosities from 10$^{41}$ to over 10$^{44}$ erg s$^{-1}$. No non-rotating model radiates more than $5 \times 10^{50}$ erg of light or has a kinetic energy exceeding $5… Expand
Pulsational Pair-instability Supernovae in Very Close Binaries
Pair-instability and pulsational pair-instability supernovae (PPISN) have not been unambiguously observed so far. They are, however, promising candidates for the progenitors of the heaviest binaryExpand
Pulsational Pair-instability Supernovae. I. Pre-collapse Evolution and Pulsational Mass Ejection
We calculate the evolution of massive stars, which undergo pulsational pair-instability (PPI) when the O-rich core is formed. The evolution from the main-sequence through the onset of PPI isExpand
Related progenitor models for long-duration gamma ray bursts and Type Ic superluminous supernovae
We model the late evolution and mass loss history of rapidly rotating Wolf-Rayet stars in the mass range $5\,\rm{M}_{\odot}\dots 100\,\rm{M}_{\odot}$. We find that quasi-chemically homogeneouslyExpand
Stellar Yields of Rotating First Stars. II. Pair Instability Supernovae and Comparison with Observations
Recent theory predicts that a first star is born with a massive initial mass of $\gtrsim$ 100 $M_\odot$. Pair instability supernova (PISN) is a common fate for such a massive star. Our final goal isExpand
Hydrogen-rich supernovae beyond the neutrino-driven core-collapse paradigm
Type II supernovae are the final stage of massive stars (above 8 M⊙) which retain part of their hydrogen-rich envelope at the moment of explosion. They typically eject up to 15 M⊙ of material, withExpand
An extremely energetic supernova from a very massive star in a dense medium
The interaction of a supernova with a circumstellar medium (CSM) can dramatically increase the emitted luminosity by converting kinetic energy to thermal energy. In ‘superluminous’ supernovae of typeExpand
The Low Detection Rate of Pair–instability Supernovae and the Effect of the Core Carbon Fraction
The pair instability supernova (PISN) is a common fate of very massive stars (VMSs). Current theory predicts the initial and the CO core mass ranges for PISNe of $\sim$140-260 $M_\odot$ andExpand
Very massive stars, pair-instability supernovae and intermediate-mass black holes with the sevn code
Understanding the link between massive ($\gtrsim 30$ M$_{\odot{}}$) stellar black holes (BHs) and their progenitor stars is a crucial step to interpret observations of gravitational-wave events. InExpand
SN 2016iet: The Pulsational or Pair Instability Explosion of a Low-metallicity Massive CO Core Embedded in a Dense Hydrogen-poor Circumstellar Medium
We present optical photometry and spectroscopy of SN 2016iet, an unprecedented Type I supernova (SN) at $z=0.0676$ with no obvious analog in the existing literature. The peculiar light curve has twoExpand
The Explosion of Helium Stars Evolved with Mass Loss
Light curves, explosion energies, and remnant masses are calculated for a grid of supernovae resulting from massive helium stars that have been evolved including mass loss. These presupernova starsExpand


The Most Luminous Supernovae
Recent observations have revealed an amazing diversity of extremely luminous supernovae, seemingly increasing in radiant energy without bound. We consider here the physical limits of what existingExpand
For the initial mass range (140 M ☉ < M < 260 M ☉) stars die in a thermonuclear runaway triggered by the pair-production instability. The supernovae they make can be remarkably energetic (up to ~1053Expand
Mass ejection by pulsational pair instability in very massive stars and implications for luminous supernovae
Massive stars having a CO core of $\sim$40-60 M$_\odot$ experience pulsational pair-instability (PPI) after carbon-burning. This instability induces strong pulsations of the whole star and a part ofExpand
Massive stars that end their lives with helium cores in the range of 35-65 M ☉ are known to produce repeated thermonuclear outbursts due to a recurring pair-instability. In some of these events,Expand
The Detectability of Pair-Production Supernovae at z 6
Nonrotating, zero-metallicity stars with initial masses 140 M 260 M☉ are expected to end their lives as pair-production supernovae (PPSNe), in which an electron-positron pair-production instabilityExpand
Hydrogen-poor superluminous stellar explosions
Observations of a class of luminous supernovae whose properties cannot be explained by any of the following processes: radioactive decay of freshly synthesized elements, explosion shock in the envelope of a supergiant star, and interaction between the debris and slowly moving, hydrogen-rich circumstellar material. Expand
Pulsational pair instability as an explanation for the most luminous supernovae
It is reported that the brightest supernovae in the modern Universe arise from collisions between shells of matter ejected by massive stars that undergo an interior instability arising from the production of electron–positron pairs. Expand
The Progenitor stars of gamma-ray bursts
Those massive stars that give rise to gamma-ray bursts (GRBs) during their deaths must be endowed with an unusually large amount of angular momentum in their inner regions, 1-2 orders of magnitudeExpand
Supernova Light Curves Powered by Young Magnetars
We show that energy deposited into an expanding supernova remnant by a highly magnetic (B ~ 5 × 1014 G) neutron star spinning at an initial period of Pi ≈ 2-20 ms can substantially brighten the lightExpand
Very Low Energy Supernovae from Neutrino Mass Loss
It now seems likely that some percentage of more massive supernova progenitors do not explode by any of the currently discussed explosion mechanisms. This has led to speculation concerning theExpand