论文标题
来自低质量祖细胞的核心爆发超新星的三维模型对螃蟹的影响
Three-dimensional Models of Core-collapse Supernovae From Low-mass Progenitors With Implications for Crab
论文作者
论文摘要
我们提出了3D全球超新星模拟的非旋转低质量（〜9 MSUN）祖细胞，涵盖了从核心崩溃到弹跳和冲击复兴的整个演变，通过从恒星表面进行冲击爆发，直到几天后倒退完成。 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). LMCCSN模型中爆炸的开始是使用Vertex-prometheus代码自动建模的，而ECSN爆炸是使用Prometheus-HOTB代码中的参数中微子传输对先前自我一致模型范围内不同爆炸能量中的不同爆炸能量进行建模的。共享结构相似性的SAGB和LMCCSN祖细胞几乎具有球形爆炸，而金属很少混合到氢包膜中。第二次疏edge的LMCCSN导致高度不对称的爆炸。它显示出有效的混合和在扩展的氢包膜中的显着休克减速。这两种属性都允许快速的镍羽赶上电击，从而导致极端的冲击变形和非球面冲击突破。 <〜5x10^{ - 3} msun的后备质量对中子星（NS）质量和踢没有显着影响。然而，各向异性后代具有相当大的角度动量，并确定了新生NS的旋转。具有较少第二疏edge的LMCCSNE模型导致水动力和中微子诱导的NS踢大于40 km/s，NS自旋周期约为30毫秒，两者与出生时的蟹脉脉冲星的踢球均未大不相同。
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 <~5x10^{-3} Msun 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 LMCCSNe model with less 2nd dredge-up results in a hydrodynamic and neutrino-induced NS kick of >40 km/s and a NS spin period of ~30 ms, both not largely different from those of the Crab pulsar at birth.
