论文标题
HE-C-O混合物的分析和数值点火曲线之间的差异
The Differences between Analytical and Numerical Ignition Curve of He-C-O Mixture
论文作者
论文摘要
在本文中，我们使用大型反应网络找到具有典型的白矮星（WD）物质组成的单区核燃料的点火条件。必要但可能没有足够的爆炸条件是，核燃烧的时间尺度要比声音越过的时间尺度较小。在典型的白色矮人热力学条件下，核时尺度敏感地取决于所选的核反应网络，并且广泛使用的分析公式不足以准确确定不稳定的点火条件，其答案在完全可压缩的反应性湍流模拟中所处的答案。我们使用天体物理密码火炬对数值模拟中的核反应进行建模。我们报告由于核反应网络的大小引起的差异。我们的发现对使用Chandrasekhar和Sub-Chandrasekhar群众的多维模拟中的流行19个物种网络获得的数值结果具有影响。我们提出了一个足够准确的温度密度（$ t-ρ$）平面的一般标准，用于给定的初始燃料，以不稳定的方式点燃。
In this paper, we use large reaction networks to find ignition conditions of single-zone nuclear fuel with compositions typical of white dwarf (WD) matter. The necessary but, possibly not sufficient condition for initiation of detonation is that the nuclear burning proceeds on smaller timescale than the sound-crossing timescale. Under typical white dwarf thermodynamic conditions, the nuclear timescale depends sensitively on the chosen nuclear reaction network, and widely-used analytical formulae are not sufficient to accurately determine unstable ignition conditions the answer to which lies in the fully compressible reactive turbulent simulations. We model the nuclear reactions in the numerical simulation using the astrophysical code TORCH. We report the differences introduced due to the size of the nuclear reaction network. Our findings have implications for numerical results obtained using the popular 19-species network in multidimensional simulations of WD of Chandrasekhar and sub-Chandrasekhar masses. We present a sufficiently accurate general criterion in temperature-density ($T-ρ$) plane for a given initial fuel to ignite in an unstable fashion.
