ON VARIATIONS OF PRE-SUPERNOVA MODEL PROPERTIES
ON VARIATIONS OF PRE-SUPERNOVA MODEL PROPERTIES
复制标题
超新星爆发前模型性质的变化
DOI：
10.3847/1538-4365/227/2/22
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
F. Timmes
中科院分区：
文献类型：
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作者：
R. Farmer;C. Fields;C. Fields;C. Fields;I. Petermann;I. Petermann;L. Dessart;M. Cantiello;B. Paxton;F. Timmes;F. Timmes
我们探讨的变化，单星15-30，非旋转，太阳金属丰度，前超新星梅萨模型，这是由于在一个完全耦合的核反应网络中的同位素数量的变化和质量分辨率的调整。在这个二维平面内，我们定量详细的范围内的核心质量在不同阶段的演变，质量位置的主要核燃烧壳，电子分数分布，质量分数分布，燃烧寿命，恒星寿命，和紧凑性参数在核心崩溃的模型和没有质量损失。直到碳燃烧，我们通常发现质量分辨率对变化的影响比同位素的数量更大，而同位素的数量在决定氖，氧和硅燃烧的变化范围方面起着更重要的作用。质量分辨率的选择占主导地位的中间对流区和二次对流区的结构的变化，在核心和外壳氢燃烧，分别在那里，我们发现，一个最小的质量分辨率为0.01是必要的，以实现收敛的氦核心质量在0.5%的水平。另一方面，在核心坍缩开始时，我们发现中心电子分数和主要核燃烧壳层的质量位置有30%的变化，需要至少127个同位素才能使这些值收敛到10%的水平。
We explore the variation in single-star 15–30 , nonrotating, solar metallicity, pre-supernova MESA models that is due to changes in the number of isotopes in a fully coupled nuclear reaction network and adjustments in the mass resolution. Within this two-dimensional plane, we quantitatively detail the range of core masses at various stages of evolution, mass locations of the main nuclear burning shells, electron fraction profiles, mass fraction profiles, burning lifetimes, stellar lifetimes, and compactness parameter at core collapse for models with and without mass-loss. Up to carbon burning, we generally find that mass resolution has a larger impact on the variations than the number of isotopes, while the number of isotopes plays a more significant role in determining the span of the variations for neon, oxygen, and silicon burning. Choice of mass resolution dominates the variations in the structure of the intermediate convection zone and secondary convection zone during core and shell hydrogen burning, respectively, where we find that a minimum mass resolution of ≈0.01 is necessary to achieve convergence in the helium core mass at the ≈5% level. On the other hand, at the onset of core collapse, we find ≈30% variations in the central electron fraction and mass locations of the main nuclear burning shells, a minimum of ≈127 isotopes is needed to attain convergence of these values at the ≈10% level.
DOI：
10.1051/0004-6361/201526302
发表时间：
2015
期刊：
arXiv: Solar and Stellar Astrophysics
影响因子：
--
作者：
Petermann I;Langer N;Castro N;Fossati L
通讯作者：
Fossati L