贫金属星重元素丰度的核合成过程研究  

Heavy Element Abundances in Metal-poor Stars

作　　者：谢革英[1] 王浩森 王树平[1] 李宏杰[2] XIE Ge-ying;WANG Hao-sen;WANG Shu-ping;LI Hong-jie(Hebei Institute of Architecture Civil Engineering;Hebei University of Science and Technology)

机构地区：[1]河北建筑工程学院数理系,河北张家口070524 [2]河北科技大学理学院,石家庄050018

出　　处：《河北建筑工程学院学报》2018年第1期133-136,共4页Journal of Hebei Institute of Architecture and Civil Engineering

基　　金：河北省科技计划项目(15210912);张家口市科学技术研究与发展计划项目(1611064B)

摘　　要：贫金属星的元素丰度随着观测技术的提高,数据越来越丰富,为贫金属星的元素核合成理论和星系化学演化的研究提供了重要条件.以三种中子俘获核重元素观测丰度值为约束,分析了部分贫金属星重元素丰度三种核合成过程的贡献.结果显示,恒星金属丰度越接近于太阳系,其不同核合成过程对重元素丰度的贡献就与太阳系的情况越接;金属丰度较低的恒星,m-s过程对元素丰度的贡献越小,较重的元素丰度贡献主要来自r-过程.Based on a large number of observational data of element abundances in metal-poor stars,which provid clues to observe constraints on the theory of stellar nucleosynthesis of heavy elements and chemical evolution of galaxies.In this paper,the observed data of three typical elements(Sr、Ba、Eu)abundances in metal-poor stars of different metallicities are chosen.It show that that,regarding the stars with similar metallicity as the sun([Fe/H]>-2),the contribution of three kind of nature-capture processes on their heavy-elements abundance distribution is also similar to that of the sun,while the heavy elements of metal-poor stars([Fe/H]<-2)are mainly produced in rapid nature-capture process.

关 键 词：星系:丰度 物理数据与过程:核反应 核合成 恒星:基本参数 

分 类 号：P144[天文地球—天体物理]