论文标题
中等质量原始质量的核合成屈服与极贫困的恒星
Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars
论文作者
论文摘要
简略。我们的目的是更好地表征进化和命运，并确定原始质量和EMP金属性之间的中间质量恒星的更新核合成产量（z = 1E-10、1e-10、1e-8、1e-7、1e-7、1e-6和1e-5）。我们还探测了在渐近巨型分支（AGB）期间最古老的中间质量恒星的核合成中的不确定性。我们使用Monash-Mount-Mount-Mount Stromlo Stellar Evolution Code Monstar分析了模型从其主要序列（TP-AGB）从其主要序列（TP-AGB）分析到其进化的最新阶段。结果是用代码季风后加工的，该代码允许确定77种高达62NI的核合成产量。正如以前的作品中报道的那样，我们在最低质量最低Z模型中确定了质子摄入发作（PIE）。 Z = 1E-10和Z = 1E-8的模型在狭窄的初始质量范围内，大约5 msun经历了热脉冲的停止，而最终的命运是I1/2型超新星的最终命运。大约6-7个MSUN的所有初始质量模型都经历了腐蚀性的第二挖土，并在其信封中经历了显着的金属富集。这使他们能够开发出类似于太阳能的TP-AGB或TP-SUPER-AGB，最终成为白矮人。除了停止热脉冲的人外，我们的所有模型都显示出有效的第三疏and和热底燃烧的核合成特征，并激活了Nena循环和MGALSI链。这导致创建了大量的CNO，具有典型的[N/Fe]> 4），并创建了特征性的丰度签名[N/FE]> [C/FE]> [O/Fe]。由于输入物理学的差异（主要与对流和对流边界有关），我们的核合成产量与文献中存在的最新结果相对于类似金属率的中间质量模型存在巨大差异。
Abridged. We aim to better characterise the evolution and fates, and determine updated nucleosynthetic yields of intermediate-mass stars between primordial and EMP metallicity (Z=1e-10, 1e-8, 1e-7, 1e-6 and 1e-5). We also probed uncertainties in the nucleosynthesis of the oldest intermediate-mass stars during the asymptotic giant branch (AGB) phase. We analysed the evolution of models from their main sequence, through the thermally pulsing AGB (TP-AGB), to the latest stages of their evolution, using the Monash-Mount Stromlo stellar evolution code MONSTAR. The results were post-processed with the code MONSOON, which allowed for the determination of the nucleosynthetic yields of 77 species up to 62Ni. As reported in former works, we identified proton ingestion episodes (PIEs) in our lowest-mass lowest-Z models. Models of Z=1e-10 and Z=1e-8 in a narrow initial mass range around 5 Msun experience the cessation of thermal pulses, and their final fates as type-I1/2 supernovae cannot be discarded. All the models of initial mass of about 6-7 Msun experience a corrosive second dredge-up and undergo significant metal enrichment in their envelopes. This allows them to develop a solar-like TP-AGB or TP-super-AGB, ultimately becoming white dwarfs. Except for those undergoing the cessation of thermal pulses, all of our models show the nucleosynthetic signatures of both efficient third dredge-up and hot-bottom burning, with the activation of the NeNa cycle and the MgAlSi chains. This leads to the creation of vast amounts of CNO, with typical [N/Fe] > 4), and the characteristic abundance signature [N/Fe] > [C/Fe] > [O/Fe]. Due to differences in input physics (mostly related to convection and convective boundaries), our nucleosynthetic yields present dramatic differences with respect to recent results existing in the literature for intermediate-mass models of similar metallicities.
