15-40太阳质量原始超新星在贫金属星上的核合成印记
The Nucleosynthetic Imprint of 15-40 Solar Mass Primordial Supernovae on Metal-Poor Stars
摘要：
在恒星演化中加入旋转诱导混合可以改变超新星前恒星的结构和组成。我们调查祖旋转的影响，在人口III和II超新星核合成产量使用新的自适应网格细化（AMR）代码CASTRO。我们研究了Z = 0和太阳金属丰度为10^-4的15、25和40颗太阳质量恒星的球形爆炸，其中有三种爆炸能量和两种旋转速率。Z = 0模型的自转导致了初级氮的产生和更强的氢燃烧壳层，导致所有模型都以红超巨星的形式死亡。另一方面，包含自转的Z=10^-4太阳金属丰度模型以致密的蓝色恒星结束了它们的生命。由于它们的扩展结构，流体动力学比Z = 10^-4模型更有利于无金属恒星的混合和更少的回落。正如预期的那样，较高能量的爆炸比较低能量的爆炸产生更多的浓缩和更少的回落，质量较小的恒星产生更多的浓缩，留下更小的残留物。我们将我们的核合成产额与目前发现的三颗铁元素最贫乏的恒星的化学丰度进行了比较，并再现了其中一颗恒星的丰度模式，即HE 0557-4840，它的金属丰度为零，质量为15太阳质量，为2.4 x 10^51尔格超新星。假设包含15颗太阳质量的恒星，我们对Z=0模型（爆炸能量为2.4x10^51尔格或更小）的产额进行的Salpeter IMF平均积分与在更大的极端贫金属恒星样本中观测到的丰度非常一致。由于极贫金属恒星的丰度模式可能来自祖先的代表性样本，我们的产量表明，低质量超新星为早期宇宙贡献了大部分金属。
英文摘要：
The inclusion of rotationally-induced mixing in stellar evolution can alter the structure and composition of presupernova stars. We survey the effects of progenitor rotation on nucleosynthetic yields in Population III and II supernovae using the new adaptive mesh refinement (AMR) code CASTRO. We examine spherical explosions in 15, 25 and 40 solar mass stars at Z = 0 and 10^-4 solar metallicity with three explosion energies and two rotation rates. Rotation in the Z = 0 models resulted in primary nitrogen production and a stronger hydrogen burning shell which led all models to die as red supergiants. On the other hand, the Z=10^-4 solar metallicity models that included rotation ended their lives as compact blue stars. Because of their extended structure, the hydrodynamics favors more mixing and less fallback in the metal free stars than the Z = 10^-4 models. As expected, higher energy explosions produce more enrichment and less fallback than do lower energy explosions, and less massive stars produce more enrichment and leave behind smaller remnants than do more massive stars. We compare our nucleosynthetic yields to the chemical abundances in the three most iron-poor stars yet found and reproduce the abundance pattern of one, HE 0557-4840, with a zero metallicity 15 solar mass, 2.4 x 10^51 erg supernova. A Salpeter IMF averaged integration of our yields for Z=0 models with explosion energies of 2.4x10^51 ergs or less is in good agreement with the abundances observed in larger samples of extremely metal-poor stars, provided 15 solar mass stars are included. Since the abundance patterns of extremely metal-poor stars likely arise from a representative sample of progenitors, our yields suggest that low-mass supernovae contributed the bulk of the metals to the early universe.
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