论文标题
核心爆炸超新星的爆炸机制：Si/O界面的作用
Explosion mechanism of core-collapse supernovae: role of the Si/O interface
论文作者
论文摘要
我们提出了一个简单的标准，可以根据崩溃前的密度和熵曲线来预测大型恒星的爆炸性。如果在SI/SI-O接口附近存在明显的密度跳跃，则可能会爆炸。我们通过使用$ \ sim 1300 $ 1D模拟来开发定量标准，其中$ν$驱动的湍流是通过时间依赖的混合长度理论包括在内的。该标准正确地标识了超过$ 90 \％$的时间的结果。我们还发现，该标准在两种不同的祖细胞上的执行方式没有区别，使用两个不同的恒星进化代码进化：Franec和Kepler。两组祖细胞的质量函数的爆炸性大不相同：（i）恒星进化处方中的不确定性会影响超新星爆炸的预测； （ii）影响爆炸性的爆发前祖细胞的最重要特性是其密度和熵曲线。我们强调了$ν$驱动的湍流通过将我们的结果与以前的作品进行比较而在爆炸中发挥作用的重要性。
We present a simple criterion to predict the explodability of massive stars based on the density and entropy profiles before collapse. If a pronounced density jump is present near the Si/Si-O interface, the star will likely explode. We develop a quantitative criterion by using $\sim 1300$ 1D simulations where $ν$-driven turbulence is included via time-dependent mixing-length theory. This criterion correctly identifies the outcome of the supernova more than $90 \%$ of the time. We also find no difference in how this criterion performs on two different sets of progenitors, evolved using two different stellar evolution codes: FRANEC and KEPLER. The explodability as a function of mass of the two sets of progenitors is very different, showing: (i) that uncertainties in the stellar evolution prescriptions influence the predictions of supernova explosions; (ii) the most important properties of the pre-collapse progenitor that influence the explodability are its density and entropy profiles. We highlight the importance that $ν$-driven turbulence plays in the explosion by comparing our results to previous works.
