Study of Neutron-Capture Element Abundances in Metal-Poor Stars

• Published in: arXiv.org 2013-01
• Main Authors: Li, Hongjie, Shen, Xiaojing, Liang, Shuai, Cui, Wenyuan, Zhang, Bo
• Format: Article
• Language: English
• Subjects: Abundance; Constraint modelling; Iron; Metallicity; Nuclear capture; Organic chemistry; Solar system; Stars
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1301.6097

This work describes a study of elemental abundances for 30 metal-poor stars whose chemical abundances provide excellent information for setting constraints on models of neutron-capture processes. Based on the abundances of main r- and weak r-process stars, the abundance patterns of main r-process and weak r-process are obtained. The two r-process component coefficients are defined to determine the relative contributions from individual neutron-capture process to abundances of metal-poor stars. Based on the component coefficients, we find that metal-poor stars BD+4 2621 and HD 4306 are also weak r-process stars, which means that the abundance pattern produced by weak r-process is stable. All metal-poor star abundances contain the contributions of both main r-process and weak r-process. The elements produced by weak r-process have increased along with Fe over the polluted history. Most of the metal-poor star abundances do not follow the pattern observed in solar system, but there is a small fraction that do. For the low-[Sr/Fe] star BD-18 5550 ([Sr/Fe]\(\lesssim-1\)), neutron-capture element abundances can be explained by the mixture of two r-process components. Since lighter elements in this star cannot be fitted by the two components, the abundance pattern of P-component is estimated from those abundances.