论文标题
核心爆发超新星残留的婴儿期
The infancy of core-collapse supernova remnants
论文作者
论文摘要
我们提出了与Prometheus-HOTB代码的中微子驱动的超新星（SNE）的3D流体动力模拟，从而从冲击突破中演变出不对称的射出射出，直到它们在大约一年后达到同源膨胀阶段。我们的计算继续对Wongwathanarat等人的两个红色超级巨人（RSG）和两个蓝色超级巨星（BSG）祖细胞进行了模拟，后者研究了爆炸过程中第一秒爆炸及其后来的爆炸过程中的流体动力学不稳定性的爆炸不对称的增长及其后来由Rayleigh-Taylor Insteribility散发出来的。我们专注于由于$^{56} $ ni的放射性衰减而引起的延迟加速度和弹出量的通货膨胀，从而使$^{56} $ fe以及新的向外移动冲击形成，当He/h-shell界面从He/H-Shell界面引起的震动时，这种冲击会形成。富铁弹出的平均速度在100 km/s和350 km/s（$ \ sim $ 8-30 \％）中增加，而最快的1％的铁加速至$ \ sim $ \ sim $ 1000 km/s（$ \ $ \ sim $ \ sim $ 20-25 \％）。从1D模型中知道的“ Ni-Bubble效应”在我们的3D模型中加速了镍的大部分，并导致最初过度密度的Ni-Rich团块的充气，这会导致不足，伸展的手指，被压缩周围物质的过度密集的Skin所包围。我们还提供体积和表面填充因子以及球形谐波分析，以定量地表征Ni-Clump尺寸的光谱。我们的四个模型中有三个给出了大于0.3的体积填充因子，这与SN 1987a所建议的观察结果一致。
We present 3D hydrodynamic simulations of neutrino-driven supernovae (SNe) with the PROMETHEUS-HOTB code, evolving the asymmetrically expanding ejecta from shock breakout until they reach the homologous expansion phase after roughly one year. Our calculations continue the simulations for two red supergiant (RSG) and two blue supergiant (BSG) progenitors by Wongwathanarat et al., who investigated the growth of explosion asymmetries produced by hydrodynamic instabilities during the first second of the explosion and their later fragmentation by Rayleigh-Taylor instabilities. We focus on the late time acceleration and inflation of the ejecta caused by the heating due to the radioactive decay of $^{56}$Ni to $^{56}$Fe and by a new outward-moving shock, which forms when the reverse shock from the He/H-shell interface compresses the central part of the ejecta. The mean velocities of the iron-rich ejecta increase between 100 km/s and 350 km/s ($\sim$8-30\%), and the fastest one percent of the iron accelerates by up to $\sim$1000 km/s ($\sim$20-25\%). This 'Ni-bubble effect', known from 1D models, accelerates the bulk of the nickel in our 3D models and causes an inflation of the initially overdense Ni-rich clumps, which leads to underdense, extended fingers, enveloped by overdense skins of compressed surrounding matter. We also provide volume and surface filling factors as well as a spherical harmonics analysis to characterize the spectrum of Ni-clump sizes quantitatively. Three of our four models give volume filling factors larger than 0.3, consistent with what is suggested for SN 1987A by observations.
