摘要
以重元素核合成理论及星系化学演化理论所得结论为基础，提出了一种利用３ 种中子俘获过程的典型元素丰度观测值，研究在不同金属度下不同核合成过程对重元素丰度的贡献的方法．由此可以确定ｒ过程与ｓ过程的贡献比例，并可用此方法来计算其余重元素丰度，得到关于重元素核合成的重要信息．利用这种方法计算了贫金属星ＨＤ６２６４４ 、ＨＤ１２６２３８和ＨＤ１８４７１１ 的重元素丰度，并将计算结果与观测结果进行了比较。
Based on the observed abundances of several typical elements and the conclusions of the heavy elemental nucleosynthesis theory and the galactic chemical evolution theory, the authors suggest a method to determine the relative contributions from the individual neutron capture processes to the abundances of heavy elements in metal poor stars. With this method, the relative contribution proportions of the s and r processes are calculated and the abundances of the heavy elements in three metal poor stars HD 62644, HD 126238 and HD 184711 are obtained. The results of calculations are compared with observations, and then a discussion is made.
出处
《天文学报》
CSCD
北大核心
1999年第3期256-262,共7页
Acta Astronomica Sinica
基金
国家自然科学基金资助项目
关键词
贫金属星
金属丰度
重元素
丰度
metal poor star, metallicity, heavy element, abundance
