Revival of the fittest: exploding core-collapse supernovae from 12 to 25 M⊙
Revival of the fittest: exploding core-collapse supernovae from 12 to 25 M⊙
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适者生存：核心塌陷超新星从 12 米到 25 米爆炸
DOI：
10.1093/mnras/sty809
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发表时间：
2018
影响因子：
4.8
通讯作者：
Dolence, Joshua
中科院分区：
文献类型：
--
作者：
Vartanyan, David;Burrows, Adam;Radice, David;Skinner, M Aaron;Dolence, Joshua
我们提出了二维轴对称核心坍缩超新星模拟的结果，采用fornaxcode， 9个祖先模型跨越12至25 M⊙。其中四种模型在电子和中子的非弹性散射以及对中微子-核子散射不透明的多体修正中爆炸。我们发现，这四种模型在密度分布上都具有明显的Si-O界面，并且相应的密度下降降低了停滞激波周围的吸积速率，并促进了爆炸。非爆炸型号缺乏这种陡峭的功能，突出Si-O接口是爆炸的关键之一。此外，我们表明，所有的非爆炸模型都可以在适度改变宏观物理输入（包括适度的旋转和对落体速度的扰动）以及微物理输入（包括中微子-核子相互作用速率的合理改变）的情况下被推动到爆炸，这表明所有的模型可能都接近临界。在我们的模拟结束时，爆炸模型的能量为几× 1050erg，并且正在上升，强调需要在更大的网格上继续进行这些模拟，并且需要更长的时间来重现自然界中看到的能量。爆炸形态对爆炸能量有影响，各向同性抛射物越多，爆炸能量越大。我们没有发现轻子数发射自持续不对称的证据。最后，我们研究了原中子星（PNS）的性质，并探讨了维度在模拟中的作用。我们发现对流在PNS中产生更大的PNS半径和更大的‘ νμ ’亮度在二维与一维相比。
We present results of 2D axisymmetric core-collapse supernova simulations, employing theFornaxcode, of nine progenitor models spanning 12 to 25 M⊙. Four of the models explode with inelastic scattering off electrons and neutrons as well as the many-body correction to neutrino-nucleon scattering opacities. We show that these four models feature sharp Si–O interfaces in their density profiles, and that the corresponding dip in density reduces the accretion rate around the stalled shock and prompts explosion. The non-exploding models lack such a steep feature, highlighting the Si–O interface as one key to explosion. Furthermore, we show that all of the non-exploding models can be nudged to explosion with modest changes to macrophysical inputs, including moderate rotation and perturbations to infall velocities, as well as to microphysical inputs, including reasonable changes to neutrino-nucleon interaction rates, suggesting that all the models are perhaps close to criticality. Exploding models have energies of a few × 1050erg at the end of our simulation, and are rising, emphasizing the need to continue these simulations over larger grids and for longer times to reproduce the energies seen in nature. Morphology of the explosion contributes to the explosion energy, with more isotropic ejecta producing larger explosion energies. We do not find evidence for the Lepton-number Emission Self-sustained Asymmetry. Finally, we look at proto-neutron star (PNS) properties and explore the role of dimension in our simulations. We find that convection in the PNS produces larger PNS radii as well as greater ‘νμ’ luminosities in 2D compared to 1D.