A successful 3D core-collapse supernova explosion model
A successful 3D core-collapse supernova explosion model
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DOI：
10.1093/mnras/sty2585
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发表时间：
2018-09
影响因子：
4.8
通讯作者：
D. Vartanyan;A. Burrows;D. Radice;A. Skinner;J. Dolence
中科院分区：
文献类型：
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作者：
D. Vartanyan;A. Burrows;D. Radice;A. Skinner;J. Dolence
在本文中，我们提出了我们的三维，多群，多中微子种类的辐射/流体动力学模拟的结果，使用国家的最先进的代码F{\sc{ornax}}的终端动力学的非旋转的16-M$_{\odot}$恒星祖先的核心。该计算采用了非弹性散射的再分配，修正了中微子-核子散射率的多体相互作用的影响，近似广义相对论（包括引力红移的影响），速度依赖的频率平流，并在祖核心的初始扰动的实施。该模型在反弹后100毫秒内爆炸（接近硅氧界面通过暂时停滞的冲击吸积的时间），到模拟结束时（在这里，反弹后677毫秒），爆炸能量以2.5 × 10尔格·s的速度积累。超新星爆炸类似于一个不对称的多羽状结构，其中一个半球占主导地位。剩余的原中子星星在677毫秒时的引力质量是142万。即使在模拟的最后，爆炸在大多数立体角是伴随着一些吸积在环形部分在黄蜂般的腰部的碎片场。喷出物电子分数（Y$_e$）分布在$\sim$0.48至$\sim$0.56之间，其中大部分喷出物质量富含质子。这可能对超新星核合成有影响，并且可能对p-和$\nu$p-过程以及r-过程的第一个峰的位置有影响。喷出物的Y$_e$和质量密度的空间分布主要是在广角羽流和大规模的结构，但仍然是相当补丁。
In this paper, we present the results of our three-dimensional, multi-group, multi-neutrino-species radiation/hydrodynamic simulation using the state-of-the-art code F{\sc{ornax}} of the terminal dynamics of the core of a non-rotating 16-M$_{\odot}$ stellar progenitor. The calculation incorporates redistribution by inelastic scattering, a correction for the effect of many-body interactions on the neutrino-nucleon scattering rates, approximate general relativity (including the effects of gravitational redshifts), velocity-dependent frequency advection, and an implementation of initial perturbations in the progenitor core. The model explodes within $\sim$100 milliseconds of bounce (near when the silicon-oxygen interface is accreted through the temporarily-stalled shock) and by the end of the simulation (here, $\sim$677 milliseconds after bounce) is accumulating explosion energy at a rate of $\sim$2.5$\times$10$^{50}$ ergs s$^{-1}$. The supernova explosion resembles an asymmetrical multi-plume structure, with one hemisphere predominating. The gravitational mass of the residual proto-neutron star at $\sim$677 milliseconds is $\sim$1.42 M$_{\odot}$. Even at the end of the simulation, explosion in most of the solid angle is accompanied by some accretion in an annular fraction at the wasp-like waist of the debris field. The ejecta electron fraction (Y$_e$) is distributed from $\sim$0.48 to $\sim$0.56, with most of the ejecta mass proton-rich. This may have implications for supernova nucleosynthesis, and could have a bearing on the p- and $\nu$p-processes and on the site of the first peak of the r-process. The ejecta spatial distributions of both Y$_e$ and mass density are predominantly in wide-angle plumes and large-scale structures, but are nevertheless quite patchy.