Abstract
ABSTRACT We present 3D full-sphere supernova simulations of non-rotating low-mass (∼9 M⊙) 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 × 1050 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 second 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 $\mathord {\lesssim }\, 5\, \mathord {\times }\, 10^{-3}$ M⊙ have no significant effects on the neutron star (NS) masses and kicks. The anisotropic fallback carries considerable angular momentum, however, and determines the spin of the newly born NS. The LMCCSN model with less second dredge-up results in a hydrodynamic and neutrino-induced NS kick of >40 km s−1 and a NS spin period of ∼30 ms, both not largely different from those of the Crab pulsar at birth.
Highlights
According to current understanding, stars with initial masses of 8–9 M end their lives in a core-collapse supernova (CCSN)
We study an electron-capture supernova (ECSN) of a non-rotating 8.8 M superAGB star (e8.8), which is constructed from the envelope model of Jones et al (2013) and a collapsing core model (Leung et al 2020; Tolstov, Leung, and Nomoto, private communication), and two CCSNe resulting from non-rotating low-mass red supergiant (RSG) with iron cores (z9.6, s9.0), evolved to the onset of collapse by Heger and by Woosley & Heger (2015), respectively
VERTEX-PROMETHEUSis a hydrodynamics code based on an implementation of the piecewise parabolic method (PPM) of Colella & Woodward (1984), coupled with a three-flavour, energy-dependent, ray-by-ray-plus (RbR+) neutrino transport scheme that iteratively solves the neutrino energy and momentum equations with a closure determined from a tangent-ray Boltzmann solver
Summary
Stars with initial masses of 8–9 M end their lives in a core-collapse supernova (CCSN). In the past six decades, numerous studies have focused on the collapse phase and subsequent evolution using 1D simulations. Physics have driven our understanding of the explosion mechanism (see e.g. Janka 2012; Janka et al 2012; Burrows 2013; Janka, Melson & Summa 2016; Muller 2016). Buras et al 2006; Takiwaki, Kotake & Suwa 2012; O’Connor & Couch 2018a; Glas et al 2019a; Skinner et al 2019 and references therein) have enabled full 3D simulations of the early explosion phase Couch & O’Connor 2014; Takiwaki, Kotake & Suwa 2014; Lentz et al 2015; Melson, Janka & Marek 2015a; Melson et al 2015b; Roberts et al 2016; Summa et al 2016; Muller et al The increase of computational capabilities in the recent years along with new developments for neutrino transport methods (see e.g. Buras et al 2006; Takiwaki, Kotake & Suwa 2012; O’Connor & Couch 2018a; Glas et al 2019a; Skinner et al 2019 and references therein) have enabled full 3D simulations of the early explosion phase
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