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题名:
A statistical model for predicting the average abundance patterns of heavier elements in metal-poor stars
作者: Zhang Bo(章博); Zhang Yanxia(张彦霞); Li, J; Peng, QH
关键词: stars : abundances ; stars : Population II ; Galaxy : evolution ; method : statistical
刊名: CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS
发表日期: 2002-10-01
卷: 2, 期:5, 页:429-440
收录类别: SCI
英文摘要: We have collected nearly all the available observed data of the elements from Ba to Dy in halo and disk stars in the metallicity range -4.0 <[Fe/H]< 0.5. Based on the observed data of Ba and Eu, we evaluated the least-squares regressions of [Ba/Fe] on [Fe/H], and [Eu/H] on [Ba/H]. Assuming that the heavy elements (heavier than Ba) are produced by a combination of the main components of s- and r-processes in metal-poor stars, and choosing Ba and Eu as respective representative elements of the main s- and the main r-processes, a statistical model for predicting the Galactic chemical evolution of the heavy elements is presented. With this model, we calculate the mean abundance trends of the heavy elements La, Ce, Pr, Nd, Sm, and Dy with the metallicity. We compare our results with the observed data at various metallicities, showing that the predicted trends are in good agreement with the observed trends, at least for the metallicity range [Fe/H]greater than or equal to -2.5. Finally, we discuss our results and deduce some important information about the Galactic chemical evolution.
语种: 英语
WOS记录号: WOS:000178799000006
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内容类型: 期刊论文
URI标识: http://ir.bao.ac.cn/handle/114a11/8632
Appears in Collections:光学天文研究部_期刊论文

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作者单位: 1.Hebei Normal Univ, Dept Phys, Shijiazhuang 050016, Peoples R China
2.Natl Lab Heavy Ion Accelerator, Ctr Theoret Nucl Phys, Lanzhou 730000, Peoples R China
3.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
4.Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China

Recommended Citation:
Zhang, B,Zhang, YX,Li, J,et al. A statistical model for predicting the average abundance patterns of heavier elements in metal-poor stars[J]. CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS,2002,2(5):429-440.
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