论文标题
[RB/ZR] BA星的比例作为伴侣AGB恒星质量的诊断
[Rb/Zr] ratio in Ba stars as diagnostics of the companion AGB stellar mass
论文作者
论文摘要
了解渐近巨型分支（AGB）恒星的核合成和演变至关重要，因为它们是宇宙中一些关键要素的主要生产者。它们是缓慢中子捕获核合成的主要位点。尚未清楚地理解在AGB恒星内部发生的确切的物理条件和核合成过程，从而更好地理解了这些恒星对银河化学富集的贡献。众所周知，通过二元传质机制接收了AGB进化的产物，构成了重要的工具，以追踪AGB核合成。 [RB/ZR]比率是了解S过程位点的平均中子密度并为伴侣AGB恒星质量提供重要线索的重要诊断。在这项工作中，我们基于对BA恒星样品的高分辨率光谱分析介绍了[RB/ZR]比率的估计值，并讨论了如何使用它来理解AGB恒星的特征。还提出了基于参数模型的分析结果，以确认伴随AGB星的质量。
Understanding the nucleosynthesis and evolution of Asymptotic Giant Branch (AGB) stars is of primary importance as they are the main producers of some of the key elements in the Universe. They are the predominant sites for the slow neutron-capture nucleosynthesis. The exact physical conditions and nucleosynthetic processes occuring at the interior of AGB stars are not clearly understood, that hinders a better understanding of the contribution of these stars to the Galactic chemical enrichment. The extrinsic stars, which are known to have received products of AGB phase of evolution via binary mass transfer mechanisms, form vital tools to trace the AGB nucleosynthesis. The [Rb/Zr] ratio is an important diagnostic to understand the average neutron density at the s-process site and provide important clues to the mass of the companion AGB stars. In this work we have presented the estimate of [Rb/Zr] ratios, based on the high resolution spectroscopic analysis for a sample of Ba stars, and discussed how it can be used to understand the characteristics of the AGB star. Results from an analysis based on parametric model to confirm the mass of the companion AGB star are also presented.
