| A Statistical Model for Predicting the Average Abundance Patterns of Heavier Elements in Metal-Poor Stars |
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| 引用本文： | Bo Zhang,Yan-Xia Zhang,Ji Li and Qiu-He Peng1 Department of Physics,Hebei Normal University,Shijiazhuang 0500162 Center of Theoretical Nuclear Physics,National Laboratory of Heavy Ion Accelerator,Lanzhou 7300003 National Astronomical Observatories,Chinese Academy of Sciences,Beijing 1000124 Department of Astronomy,Nanjing University,Nanjing 210093. A Statistical Model for Predicting the Average Abundance Patterns of Heavier Elements in Metal-Poor Stars[J]. 中国天文和天体物理学报, 2002, 2(5): 429-440 |
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| 作者姓名： | Bo Zhang Yan-Xia Zhang Ji Li and Qiu-He Peng1 Department of Physics Hebei Normal University Shijiazhuang 0500162 Center of Theoretical Nuclear Physics National Laboratory of Heavy Ion Accelerator Lanzhou 7300003 National Astronomical Observatories Chinese Academy of Sciences Beijing 1000124 Department of Astronomy Nanjing University Nanjing 210093 |
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| 作者单位： | Bo Zhang，Yan-Xia Zhang，Ji Li and Qiu-He Peng1 Department of Physics，Hebei Normal University，Shijiazhuang 0500162 Center of Theoretical Nuclear Physics，National Laboratory of Heavy Ion Accelerator，Lanzhou 7300003 National Astronomical Observatories，Chinese Academy of Sciences，Beijing 1000124 Department of Astronomy，Nanjing University，Nanjing 210093 |
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| 基金项目： | This research has been supported by the National Natural Science Foundation of China through grant No.19973002，Chinese Academy of Sciences-Peking University Joint Beijing Astrophysical Center. |
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| 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]> -2.5. Finally, we discuss our results and deduce some importa
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| 关 键 词： | 统计模型 贫金属星系 重元素 丰度 镧 铈 镨 钕 钐 金属特征 银河系 |
A Statistical Model for Predicting the Average Abundance Patterns of Heavier Elements in Metal-Poor Stars |
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| Bo Zhang,Yan-Xia Zhang,Ji Li,Qiu-He Peng. 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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| Authors: | Bo Zhang Yan-Xia Zhang Ji Li Qiu-He Peng |
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| Abstract: | 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]≥ -2.5. Finally,we discuss our results and deduce some important information about the Galactic chemical evolution. |
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| Keywords: | stars: abundances - stars: Population II - Galaxy: evolution method: statistical |
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