Three-dimensional Models of Core-collapse Supernovae From Low-mass Progenitors With Implications for Crab

We present 3D full-sphere supernova simulations of non-rotating low-mass (~9 Msun) progenitors, covering the entire evolution from core collapse through bounce and shock revival, through shock breakout from the stellar surface, until fallback is completed several days later. We obtain low-energy exp...

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Bibliographic Details
Published in:arXiv.org 2020-06
Main Authors: Stockinger, G, H -Th Janka, Kresse, D, Melson, T, Ertl, T, Gabler, M, Gessner, A, Wongwathanarat, A, Tolstov, A, S -C Leung, Nomoto, K, Heger, A
Format: Article
Language:English
Subjects:
Angular momentum
Collapse
Computer simulation
Deceleration
Explosions
Magnesium
Neon
Neutrinos
Neutron stars
Progenitors (astrophysics)
Pulsars
Stellar evolution
Stellar surfaces
Supernovae
Three dimensional models
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Summary:We present 3D full-sphere supernova simulations of non-rotating low-mass (~9 Msun) progenitors, covering the entire evolution from core collapse through bounce and shock revival, through shock breakout from the stellar surface, until fallback is completed several days later. We obtain low-energy explosions [~(0.5-1.0)x 10^{50} erg] of iron-core progenitors at the low-mass end of the core-collapse supernova (LMCCSN) domain and compare to a super-AGB (sAGB) progenitor with an oxygen-neon-magnesium core that collapses and explodes as electron-capture supernova (ECSN). The onset of the explosion in the LMCCSN models is modelled self-consistently using the Vertex-Prometheus code, whereas the ECSN explosion is modelled using parametric neutrino transport in the Prometheus-HOTB code, choosing different explosion energies in the range of previous self-consistent models. The sAGB and LMCCSN progenitors that share structural similarities have almost spherical explosions with little metal mixing into the hydrogen envelope. A LMCCSN with less 2nd dredge-up results in a highly asymmetric explosion. It shows efficient mixing and dramatic shock deceleration in the extended hydrogen envelope. Both properties allow fast nickel plumes to catch up with the shock, leading to extreme shock deformation and aspherical shock breakout. Fallback masses of 40 km/s and a NS spin period of ~30 ms, both not largely different from those of the Crab pulsar at birth.
ISSN:2331-8422
DOI:10.48550/arxiv.2005.02420