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 ≲ 5×10⁻³ 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.

中文翻译：

---

来自低质量祖先的核心坍缩超新星的三维模型对蟹的影响

我们展示了非旋转低质量 (∼9 M_⊙) 前身的 3D 全球面超新星模拟，涵盖了从核心坍缩到反弹和激波复活，从恒星表面激波突破，直到几天后回落完成的整个演化过程之后。我们在核坍缩超新星 (LMCCSN) 域的低质量端获得了铁核前体的低能量爆炸 (∼0.5–1.0 × 10⁵⁰ erg)，并与具有氧的超 AGB (sAGB) 前体进行了比较-氖-镁核心，坍缩并爆炸为电子俘获超新星 (ECSN)。LMCCSN 模型中爆炸的开始使用 VERTEX-PROMETHEUS 代码自洽建模，而 ECSN 爆炸使用 PROMETHEUS-HOTB 代码中的参数中微子输运建模，在以前的自洽模型范围内选择不同的爆炸能量。具有结构相似性的 sAGB 和 LMCCSN 祖先几乎呈球形爆炸，几乎没有金属混合到氢包层中。具有较少二次疏浚的 LMCCSN 会导致高度不对称的爆炸。它在扩展的氢包层中显示出有效的混合和剧烈的冲击减速。这两种特性都允许快速镍羽流赶上冲击，导致极端冲击变形和非球面冲击爆发。回退质量 ≲ 5×10⁻³ M_⊙ 对中子星 (NS) 的质量和踢动没有显着影响。然而，各向异性回落带有相当大的角动量，并决定了新生 NS 的自旋。