利用星风吸积模型计算钡星的重元素丰度  

Calculation of Heavy-element Abundances for Ba Stars Adopting Yutaka Komiya's Model of Wind Accretion

作　　者：丁振瑞[1] 刘俊红[2] 

机构地区：[1]河北大学物理科学与技术学院,河北保定071002 [2]石家庄学院物理系,河北石家庄050035

出　　处：《河北大学学报（自然科学版）》2010年第3期247-250,共4页Journal of Hebei University(Natural Science Edition)

基　　金：河北省自然科学基金资助项目(A2008000560)

摘　　要：为进一步探讨钡星的形成机制,采用了Yutaka Komiya(2007)建立的双星星风吸积模型,计算了4颗钡星的s-元素丰度,并和观测结果作了比较.结果发现,中子辐照量在重元素核合成方面起主导作用,同时检验了Yutaka Komiya模型的合理性.In order to discuss formation mechanism of the barium stars furtherly,Yutaka Komiya＇s model of wind accretion from Jeans＇ theorems was adopted.The s-element abundances of four barium stars was calculated and compared with observation results.It found that the neutron exposure was played important role in the nucleosynthesis of heavy-element,and the reasonableness of Yutaka Komiya＇s model was checked.

关 键 词：钡星 超丰 金属丰度 中子辐照量 

分 类 号：P142.9[天文地球—天体物理]