Three-dimensional supernova explosion simulations of 9-, 10-, 11-, 12-, and 13-M · stars

Adam Burrows, David Radice, David Vartanyan

Research output: Contribution to journalArticle

4 Citations (Scopus)

Abstract

Using the new state-of-the-art core-collapse supernova (CCSN) code FORNAX, we have simulated the three-dimensional dynamical evolution of the cores of 9-, 10-, 11-, 12-, and 13-M stars from the onset of collapse. Stars from 8 to 13 M constitute roughly 50 per cent of all massive stars, so the explosive potential for this mass range is important to the overall theory of CCSNe. We find that the 9-, 10-, 11-, and 12-M models explode in 3D easily, but that the 13-M model does not. From these findings, and the fact that slightly more massive progenitors seem to explode, we suggest that there is a gap in explodability near 12 to 14 M for non-rotating progenitor stars. Factors conducive to explosion are turbulence behind the stalled shock, energy transfer due to neutrino-matter absorption and neutrino-matter scattering, many-body corrections to the neutrino-nucleon scattering rate, and the presence of a sharp silicon-oxygen interface in the progenitor. Our 3D exploding models frequently have a dipolar structure, with the two asymmetrical exploding lobes separated by a pinched waist where matter temporarily continues to accrete. This process maintains the driving neutrino luminosity, while partially shunting matter out of the way of the expanding lobes, thereby modestly facilitating explosion. The morphology of all 3D explosions is characterized by multiple bubble structures with a range of low-order harmonic modes. Though much remains to be done in CCSN theory, these and other results in the literature suggest that, at least for these lower mass progenitors, supernova theory is converging on a credible solution.

Original languageEnglish (US)
Pages (from-to)3169-3184
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Volume485
Issue number3
DOIs
StatePublished - Feb 28 2019

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M stars
supernovae
explosions
explosion
neutrinos
scattering
lobes
simulation
stars
silicon
explosive
bubble
turbulence
massive stars
oxygen
bubbles
energy transfer
shock
luminosity
harmonics

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

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title = "Three-dimensional supernova explosion simulations of 9-, 10-, 11-, 12-, and 13-M · stars",
abstract = "Using the new state-of-the-art core-collapse supernova (CCSN) code FORNAX, we have simulated the three-dimensional dynamical evolution of the cores of 9-, 10-, 11-, 12-, and 13-M stars from the onset of collapse. Stars from 8 to 13 M constitute roughly 50 per cent of all massive stars, so the explosive potential for this mass range is important to the overall theory of CCSNe. We find that the 9-, 10-, 11-, and 12-M models explode in 3D easily, but that the 13-M model does not. From these findings, and the fact that slightly more massive progenitors seem to explode, we suggest that there is a gap in explodability near 12 to 14 M for non-rotating progenitor stars. Factors conducive to explosion are turbulence behind the stalled shock, energy transfer due to neutrino-matter absorption and neutrino-matter scattering, many-body corrections to the neutrino-nucleon scattering rate, and the presence of a sharp silicon-oxygen interface in the progenitor. Our 3D exploding models frequently have a dipolar structure, with the two asymmetrical exploding lobes separated by a pinched waist where matter temporarily continues to accrete. This process maintains the driving neutrino luminosity, while partially shunting matter out of the way of the expanding lobes, thereby modestly facilitating explosion. The morphology of all 3D explosions is characterized by multiple bubble structures with a range of low-order harmonic modes. Though much remains to be done in CCSN theory, these and other results in the literature suggest that, at least for these lower mass progenitors, supernova theory is converging on a credible solution.",
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Three-dimensional supernova explosion simulations of 9-, 10-, 11-, 12-, and 13-M · stars . / Burrows, Adam; Radice, David; Vartanyan, David.

In: Monthly Notices of the Royal Astronomical Society, Vol. 485, No. 3, 28.02.2019, p. 3169-3184.

Research output: Contribution to journalArticle

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AB - Using the new state-of-the-art core-collapse supernova (CCSN) code FORNAX, we have simulated the three-dimensional dynamical evolution of the cores of 9-, 10-, 11-, 12-, and 13-M stars from the onset of collapse. Stars from 8 to 13 M constitute roughly 50 per cent of all massive stars, so the explosive potential for this mass range is important to the overall theory of CCSNe. We find that the 9-, 10-, 11-, and 12-M models explode in 3D easily, but that the 13-M model does not. From these findings, and the fact that slightly more massive progenitors seem to explode, we suggest that there is a gap in explodability near 12 to 14 M for non-rotating progenitor stars. Factors conducive to explosion are turbulence behind the stalled shock, energy transfer due to neutrino-matter absorption and neutrino-matter scattering, many-body corrections to the neutrino-nucleon scattering rate, and the presence of a sharp silicon-oxygen interface in the progenitor. Our 3D exploding models frequently have a dipolar structure, with the two asymmetrical exploding lobes separated by a pinched waist where matter temporarily continues to accrete. This process maintains the driving neutrino luminosity, while partially shunting matter out of the way of the expanding lobes, thereby modestly facilitating explosion. The morphology of all 3D explosions is characterized by multiple bubble structures with a range of low-order harmonic modes. Though much remains to be done in CCSN theory, these and other results in the literature suggest that, at least for these lower mass progenitors, supernova theory is converging on a credible solution.

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