Kifonidis K, Plewa T, Janka H, Müller E
Astrophys J. 2000 Mar 10;531(2):L123-L126. doi: 10.1086/312541.
High-resolution two-dimensional simulations were performed for the first 5 minutes of the evolution of a core-collapse supernova explosion in a 15 M middle dot in circle blue supergiant progenitor. The computations start shortly after bounce and include neutrino-matter interactions by using a lightbulb approximation for the neutrinos and a treatment of the nucleosynthesis due to explosive silicon and oxygen burning. We find that newly formed iron-group elements are distributed throughout the inner half of the helium core by Rayleigh-Taylor instabilities at the (Ni + Si)/O and (C + O)/He interfaces, seeded by convective overturn during the early stages of the explosion. Fast-moving nickel mushrooms with velocities up to approximately 4000 km s-1 are observed. This offers a natural explanation for the mixing required in light-curve and spectral synthesis studies of Type Ib explosions. A continuation of the calculations to later times, however, indicates that the iron velocities observed in SN 1987A cannot be reproduced because of a strong deceleration of the clumps in the dense shell left behind by the shock at the He/H interface.
针对一颗15 M⊙蓝超巨星前身星核心坍缩超新星爆发演化的前5分钟进行了高分辨率二维模拟。计算在反弹后不久开始，通过对中微子采用点源近似以及对爆炸硅和氧燃烧导致的核合成进行处理，包含了中微子与物质的相互作用。我们发现，新形成的铁族元素通过（Ni + Si）/O和（C + O）/He界面处的瑞利 - 泰勒不稳定性分布在氦核的内半部，这是由爆炸早期阶段的对流翻转引发的。观测到速度高达约4000 km s-1的快速移动镍团块。这为Ib型超新星爆发的光变曲线和光谱合成研究中所需的混合提供了一种自然解释。然而，将计算延续到更晚的时间表明，由于在He/H界面处激波留下的致密壳层中团块的强烈减速，无法再现1987A超新星中观测到的铁速度。
