钡星是慢中子俘获过程元素超丰的恒星，其增丰的原因被广泛认为是由于遭受到它们的白矮星伴星的前身星在AGB阶段抛射物质的污染。钡星慢中子俘获过程元素丰度的测定可以为AGB星中子俘获核合成的研究提供观测上的约束，同时为更好的理解其对银河系化学增丰所做的贡献提供证据。. 有关钡星的研究已持续近七十年，但是有关钡星的形成机制及演化特性仍未被充分理解且缺乏定论，一个重要原因是钡星、尤其是钡矮星的样本极少，限制了对其深入研究。LAMOST刚刚开始的中分辨率光谱巡天可以为发现更多的钡星提供光谱数据，也为进一步研究钡星的起源与特性提供了条件。本课题的主要工作包括：1. Kepler天区钡星的搜寻与证认；2. 钡巨星与钡矮星性质分析及演化关系研究；3. 双星系统的轨道周期、白矮星伴星质量及偏心率等参数对钡星成因及慢中子俘获过程元素增丰程度的影响。

Barium stars are chemically peculiar stars whose envelopes exhibit overabundance of s-process elements, and the enhancement materials are generally believed to come from the mass transfer from their AGB companions (now WD). Detailed chemical abundances of s-process elements can provide observational constraints for the studies of neutron-capture nucleosynthesis and clues for understanding their contribution to the Galactic chemical enrichment..The studies on barium stars have continued nearly 70 years, but the formation mechanism and evolution properties still are not understood. One important reason is that the number of barium stars, especially barium dwarf stars, is very small, which hinders the study of these stars. The medium-resolution spectra survey of LAMOST will produce massive spectra, which provides data source and good condition for finding more barium stars and further research. The main work of this research includes: 1. Search for and identify the barium stars; 2. Analyze the properties of barium giants and barium dwarfs, and study the relation between them. 3. The influence of the orbital period, the mass of white dwarf and the eccentricity on the origin and the level of s-process overabundance among barium stars.