The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations

Journal Article · 28 November 2019 · Monthly Notices of the Royal Astronomical Society

DOI: https://doi.org/10.1093/mnras/stz3223 · OSTI ID:1643757

Burrows, Adam ^[1]; Radice, David  ^[2]; Vartanyan, David ^[1]; Nagakura, Hiroki ^[1]; Skinner, M Aaron ^[3]; Dolence, Joshua C ^[4]

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1. Princeton Univ., NJ (United States)
2. Princeton Univ., NJ (United States); Pennsylvania State Univ., University Park, PA (United States)
3. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
4. Los Alamos National Lab. (LANL), Los Alamos, NM (United States)

We have conducted 19 state-of-the-art 3D core-collapse supernova simulations spanning a broad range of progenitor masses. This is the largest collection of sophisticated 3D supernova simulations ever performed. We have found that while the majority of these models explode, not all do, and that even models in the middle of the available progenitor mass range may be less explodable. This does not mean that those models for which we did not witness explosion would not explode in Nature, but that they are less prone to explosion than others. One consequence is that the ‘compactness’ measure is not a metric for explodability. We find that lower-mass massive star progenitors likely experience lower-energy explosions, while the higher-mass massive stars likely experience higher-energy explosions. Moreover, most 3D explosions have a dominant dipole morphology, have a pinched, wasp-waist structure, and experience simultaneous accretion and explosion. We reproduce the general range of residual neutron-star masses inferred for the galactic neutron-star population. The most massive progenitor models, however, in particular vis à vis explosion energy, need to be continued for longer physical times to asymptote to their final states. We find that while the majority of the inner ejecta have Ye = 0.5, there is a substantial proton-rich tail. This result has important implications for the nucleosynthetic yields as a function of progenitor. Finally, we find that the non-exploding models eventually evolve into compact inner configurations that experience a quasi-periodic spiral SASI mode. We otherwise see little evidence of the SASI in the exploding models.

• Research Organization: Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States); Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
• Sponsoring Organization: Extreme Science and Engineering Discovery Environment (XSEDE); National Science Foundation (NSF); USDOE Laboratory Directed Research and Development (LDRD) Program; USDOE National Nuclear Security Administration (NNSA)
• Grant/Contract Number: 89233218CNA000001; AC02-06CH11357; AC03-76SF00098; AC52-07NA27344; SC0018297
• OSTI ID: 1643757
• Report Number(s): LA-UR--19-28512; LLNL-JRNL--787982; 986006
• Journal Information: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 2 Vol. 491; ISSN 1365-2966; ISSN 0035-8711
• Publisher: Royal Astronomical SocietyCopyright Statement
• Country of Publication: United States
• Language: English