核心坍缩超新星遗迹的幼年期
The infancy of core-collapse supernova remnants
摘要：
我们提出了三维流体动力学模拟中微子驱动的超新星（SNe）与PROMETHEUS-HOTB代码，从冲击爆发，直到他们达到同源膨胀阶段后，大约一年的不对称膨胀喷出物。我们的计算延续了Wongwathanarat等人对两颗红超巨星（RSG）和两颗蓝超巨星（BSG）祖星的模拟，他研究了在爆炸的第一秒期间由流体动力学不稳定性产生的爆炸不对称性的增长以及随后由瑞利-泰勒不稳定性产生的碎片化。我们专注于后期的时间加速和膨胀的喷出物所造成的加热由于放射性衰变的$^{56}$ Ni到$^{56}$ Fe和一个新的向外移动的冲击，形成时，从He/H壳层界面的反向冲击压缩的中央部分的喷出物。富铁喷出物的平均速度在100 km/s和350 km/s之间增加（$\sim$ 8-30\%），最快的百分之一的铁加速到$\sim$ 1000 km/s（$\sim$ 20-25\%）。从1D模型中已知的这种“镍气泡效应”加速了我们3D模型中的镍块，并导致最初过密的富镍团块膨胀，这导致密度不足，延伸的手指，被压缩周围物质的过密皮肤包裹。我们还提供了体积和表面填充因子，以及一个球谐函数分析，以表征光谱的镍块大小定量。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 1987 A的观测结果一致。
英文摘要：
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.
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