Three-dimensional Core-collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout
Three-dimensional Core-collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout
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DOI：
10.3847/1538-4357/ac1d49
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发表时间：
2021-06
期刊：
影响因子：
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通讯作者：
M. A. Sandoval;W. Hix;O. E. Bronson Messer;E. Lentz;J. A. Harris
中科院分区：
文献类型：
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作者：
M. A. Sandoval;W. Hix;O. E. Bronson Messer;E. Lentz;J. A. Harris
我们提出了三维模拟的核心坍缩超新星使用FLASH代码，按照爆炸的进展到恒星表面，从中微子辐射流体动力学模拟的中微子驱动阶段进行的奇美拉代码。我们考虑从2D和3D嵌合体模型开始的9.6 M的零金属量祖先和从2D嵌合体模型开始的10 M的太阳金属量祖先，所有模拟直到3D中的冲击爆发，同时跟踪160个核素。超新星激波和富含金属的瑞利-泰勒（R-T）“子弹”之间的相对速度差异决定了富含金属的喷出物在传播通过祖先的密度分布时如何演变，并决定了爆炸的最终形态。我们发现，在二维和三维9.6 M嵌合体模型中，由于子弹穿透He/H壳的能力，56 Ni在冲击波爆发时的最大速度分别为1950和1750 km s−1。当从2D映射时，我们发现当2D Chimera模型和3D FLASH模型网格对齐时，高速结构的发展被抑制。快速增长的球形气泡结构的发展，而不是缓慢增长的环形结构所施加的轴对称，允许相互作用的子弹与冲击和种子进一步的R-T不稳定性在He/H界面。我们在10 M反冲模型中看到了类似的效应，它在冲击爆发时达到了最大56 Ni速度为2500 km s−1。
We present three-dimensional simulations of core-collapse supernovae using the FLASH code that follow the progression of the explosion to the stellar surface, starting from neutrino radiation hydrodynamic simulations of the neutrino-driven phase performed with the Chimera code. We consider a 9.6 M ☉ zero-metallicity progenitor starting from both 2D and 3D Chimera models and a 10 M ☉ solar-metallicity progenitor starting from a 2D Chimera model, all simulated until shock breakout in 3D while tracking 160 nuclear species. The relative velocity difference between the supernova shock and the metal-rich Rayleigh–Taylor (R-T) “bullets” determines how the metal-rich ejecta evolves as it propagates through the density profile of the progenitor and dictates the final morphology of the explosion. We find maximum 56Ni velocities of ∼1950 and ∼1750 km s−1 at shock breakout from 2D and 3D 9.6 M ☉ Chimera models, respectively, due to the bullets’ ability to penetrate the He/H shell. When mapping from 2D, we find that the development of higher-velocity structures is suppressed when the 2D Chimera model and 3D FLASH model meshes are aligned. The development of faster-growing spherical-bubble structures, as opposed to the slower-growing toroidal structure imposed by axisymmetry, allows for interaction of the bullets with the shock and seeds further R-T instabilities at the He/H interface. We see similar effects in the 10 M ☉ model, which achieves maximum 56Ni velocities of ∼2500 km s−1 at shock breakout.