金属丰度对中子俘获过程影响的元素丰度分解研究

对大量不同金属丰度恒星的化学丰度研究，可加深对中子俘获核合成过程与星系化学演化的一系列天体物理重要前沿问题的理解。本项目将对各种金属丰度的恒星（包括球状星团恒星）丰度观测资料（包括轻元素、铁族元素及中子俘获元素）进行细致分类，全面分析比较，从中提取更多与s-过程和r-过程核合成密切相关的物理信息。将中子俘获元素丰度分析与轻元素、铁族元素丰度分析有机结合起来，得到与各中子俘获过程对应、包括中子俘获元素及伴随抛出元素在内的元素丰度分布曲线，建立恒星中子俘获元素丰度的四分量（主要s-、弱s-、主要r-和弱r-过程）完备模型，确定银河系中各类恒星丰度中不同中子俘获过程相对贡献，从而加深金属丰度对各个中子俘获核合成过程影响的理解，解决一些关于中子俘获元素核合成及星系化学演化的重要问题。将近邻矮星系恒星元素丰度定量分解，为近邻矮星系恒星形成历史、恒星内部核合成特征和化学演化的研究提供更多约束。

The research on the chemical abundances of stars with various metallicities could give us further understanding of the important astrophysical issues about neutron-capture nucleosynthesis and the Galactic chemical evolution. In this project, based on the comprehensive analysis and comparison, we will make detailed classification of the observational abundances (including the abundances of light elements, iron group elements and neutron-capture elements) of stars with various metallicities (including the globular cluster stars), in order to extract more physical information tightly related to the s-process and r-process nucleosynthesis. Through analyzing the abundances of neutron-capture elements together with light elements and iron group elements, we can obtain the abundance curves, including the neutron-capture elements and the light elements ejected with them, of individual neutron-capture process. We will set up the complete model of four components (the main s-, weak s-, main r- and weak r-process) and sequentially determine the relative contribution from individual neutron-capture process to the element abundances of the stars with various metallicities, which can promote us to better understand the effect of metallicity to each neutron-capture process and solve some important problems about neutron-capture nucleosynthesis and the Galactic chemical evolution. Through quantitative decomposition of the element abundances for the stars in nearby dwarf galaxies, our work would provide the more constraints to the theories of stellar formation histories, the nucleosynthesis characteristics and galaxy chemical evolution.