STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS
STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS
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富含金属的渐近巨分支模型的出色产量
DOI：
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发表时间：
2016
期刊：
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通讯作者：
M. Lugaro
中科院分区：
文献类型：
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作者：
A. Karakas;M. Lugaro
我们提出了富含金属的渐近巨星分支（AGB）模型的三个网格的新理论恒星产量和表面丰度。对于 Z = 0.007 时初始质量在 1 M☉ 和 7.5 M☉ 之间的恒星模型以及 Z = 0.014（太阳）和 Z = 0.03 时初始质量在 1 M☉ 和 8 M☉ 之间的恒星模型，给出了后处理核合成结果。我们将恒星表面丰度作为 AGB 上从 C 到 Bi 的元素的热脉冲的函数，以及选择直至 Fe 和 Ni 的元素同位素比（例如 / ），这可以通过对恒星分子的观测和对陨石星尘颗粒的实验室分析来获得。还包括 He/H、C/O 和 N/O 的元素丰度比率，这对于直接比较 AGB 恒星及其后代（包括行星状星云）的观测非常有用。网格中每个模型的综合元素恒星产率均显示为氢、氦以及从 C 到 Bi 的所有稳定元素。热底燃烧的中等质量模型的锂产率也包括在内。我们提出了 Z = 0.03 的超太阳金属丰度 AGB 恒星的第一个慢中子俘获（s 过程）产率，以及在所有三种金属丰度下质量超过 6 M☉ 的模型的第一个完整的 s 过程产率。
We present new theoretical stellar yields and surface abundances for three grids of metal-rich asymptotic giant branch (AGB) models. Post-processing nucleosynthesis results are presented for stellar models with initial masses between 1 M☉ and 7.5 M☉ for Z = 0.007, and 1 M☉ and 8 M☉ for Z = 0.014 (solar) and Z = 0.03. We include stellar surface abundances as a function of thermal pulse on the AGB for elements from C to Bi and for a selection of isotopic ratios for elements up to Fe and Ni (e.g., / ), which can be obtained from observations of molecules in stars and from the laboratory analysis of meteoritic stardust grains. Ratios of elemental abundances of He/H, C/O, and N/O are also included, which are useful for direct comparison to observations of AGB stars and their progeny, including planetary nebulae. The integrated elemental stellar yields are presented for each model in the grid for hydrogen, helium, and all stable elements from C to Bi. Yields of Li are also included for intermediate-mass models with hot bottom burning. We present the first slow neutron-capture (s-process) yields for super solar metallicity AGB stars with Z = 0.03, and the first complete s-process yields for models more massive than 6 M☉ at all three metallicities.