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arXiv 1604.02178astro-ph.SRastro-ph.GA
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富金属渐近巨星分支模型的恒星产额

Stellar yields from metal-rich asymptotic giant branch models

Amanda I. Karakas, Maria Lugaro

备注：
20 pages, 20 figures, includes supplementary surface abundance and yield data tables; accepted for publication in ApJ
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摘要：

我们提出了新的理论恒星产额和表面丰度的三个网格的金属丰富的渐近巨星分支（AGB）模型。后处理核合成结果的恒星模型与初始质量之间的1 $M_{\odot}$和7.5 $M_{\odot}$的$Z=0.007$，1 $M_{\odot}$和8 $M_{\odot}$的$Z=0.014$（太阳）和$Z=0.03$。我们包括恒星表面丰度作为AGB上从C到Bi的元素的热脉冲的函数，以及Fe和Ni元素的同位素比的选择（例如，$^{12}$ C/ $^{13}$ C），它可以从恒星分子的观测和陨石星尘颗粒的实验室分析中获得。He/H、C/O和N/O的元素丰度比也包括在内，这对于与AGB星及其后代（包括行星状星云）的观测进行直接比较是有用的。在网格中给出了每个模型的氢、氦和从C到Bi的所有稳定元素的综合恒星元素产额。锂的产率也包括在热底部燃烧的中等质量模型中。我们提出了第一个$slow$中子捕获（$s$过程）产额的超太阳金属丰度AGB星与$Z=0.03$，和第一个完整的$s$过程产额的模型大于6 $M_{\odot}$在所有三个金属丰度。

英文摘要：

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$M_{\odot}$ and 7.5$M_{\odot}$ for $Z=0.007$, and 1$M_{\odot}$ and 8$M_{\odot}$ 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., $^{12}$C/$^{13}$C), 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$M_{\odot}$ at all three metallicities.

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