PROGENITOR-DEPENDENT EXPLOSION DYNAMICS IN SELF-CONSISTENT, AXISYMMETRIC SIMULATIONS OF NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE
PROGENITOR-DEPENDENT EXPLOSION DYNAMICS IN SELF-CONSISTENT, AXISYMMETRIC SIMULATIONS OF NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE
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DOI：
10.3847/0004-637x/825/1/6
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发表时间：
2015-11
期刊：
影响因子：
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通讯作者：
A. Summa;Florian Hanke;H. Janka;T. Melson;A. Marek;B. Müller
中科院分区：
文献类型：
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作者：
A. Summa;Florian Hanke;H. Janka;T. Melson;A. Marek;B. Müller
我们提出了自洽的，轴对称的核心塌陷超新星模拟进行普罗米修斯顶点代码的18个前超新星模型在11-28 M的范围内，包括最近由其他团体调查的祖先。所有的模型都会产生爆炸，但根据原型结构的不同，它们可以分为两类。随着Si/Si-O界面处密度的急剧下降，该界面到达激波前沿导致质量吸积速率的突然下降，从而触发快速接近爆炸。随着吸积速率的逐渐降低，中微子加热需要更长的时间来克服吸积冲压压力和爆炸。反弹后的高质量吸积率和相应的高中微子光度结合在Si/Si-O界面处的吸积率和冲压压力的显着下降，促进了早期的爆炸。由于快速收缩的中子星星半径和通过其最大值后的激波前沿后退，我们的模型表现出较短的平流时标，这有利于有效增长的常设吸积激波不稳定性。后者至少对失速激波在逃逸前的再膨胀起支持作用。考虑到增益层中的湍流压力的影响，我们推导出一个广义的临界中微子光度的条件，捕捉所有模型的爆炸行为非常好。我们通过测试随机性、数值分辨率和近似在微观物理学某些方面的影响来验证我们研究结果的稳健性。
We present self-consistent, axisymmetric core-collapse supernova simulations performed with the Prometheus-Vertex code for 18 pre-supernova models in the range of 11–28 M⊙, including progenitors recently investigated by other groups. All models develop explosions, but depending on the progenitor structure, they can be divided into two classes. With a steep density decline at the Si/Si–O interface, the arrival of this interface at the shock front leads to a sudden drop of the mass-accretion rate, triggering a rapid approach to explosion. With a more gradually decreasing accretion rate, it takes longer for the neutrino heating to overcome the accretion ram pressure and explosions set in later. Early explosions are facilitated by high mass-accretion rates after bounce and correspondingly high neutrino luminosities combined with a pronounced drop of the accretion rate and ram pressure at the Si/Si–O interface. Because of rapidly shrinking neutron star radii and receding shock fronts after the passage through their maxima, our models exhibit short advection timescales, which favor the efficient growth of the standing accretion-shock instability. The latter plays a supportive role at least for the initiation of the re-expansion of the stalled shock before runaway. Taking into account the effects of turbulent pressure in the gain layer, we derive a generalized condition for the critical neutrino luminosity that captures the explosion behavior of all models very well. We validate the robustness of our findings by testing the influence of stochasticity, numerical resolution, and approximations in some aspects of the microphysics.