HD 140283元素丰度分析及弱r-过程元素天体物理来源
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1.沧州师范学院物理与信息工程学院沧州061001;2.河北科技大学理学院石家庄050018;3.河北师范大学数学与信息科学学院石家庄050024;4.河北师范大学物理科学与信息工程学院石家庄050024)

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Element Abundance Analysis of HD 140283 and Astrophysics Sources of Weak r-process Elements
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1. Department of Physics and Information Engineering, Cangzhou Normal University, Cangzhou 061001;2. School of Science, Hebei University of Science and Technology, Shijiazhuang 050018;3. Department of Mathematics and Information Science, Hebei Normal University, Shijiazhuang 050024;4. Department of Physics Science and Information Engineering, Hebei Normal University, Shijiazhuang 050024;

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    摘要:

    HD 140283是一颗近邻极贫金属亚巨星, 形成于宇宙大爆炸初期, 被认为是迄今为止最古老的恒星之一, 同时它也是一颗典型的弱r-过程星, 对它的研究有助于深入理解宇宙早期演化、丰富元素核合成理论. 将HD 140283从C到Zn的观测丰度与单个超新星(SN)事件元素理论产量进行拟合, 得出HD 140283可能诞生于前身星质量为22.5\;$M_ (下标`⊙'代表太阳)的超新星爆发污染的星云. 基于同样的方法, 研究了另外5颗典型弱r-过程星, 分别得出了污染产生这些恒星的气体云的超新星前身星质量, 进一步推测了弱r-过程可能发生的天体物理环境.

    Abstract:

    HD 140283, a nearby extremely metal-poor subgiant star, formed shortly after the big bang, is thought to be the oldest star to date, and also a typical weak r-process star. Study of this star is of great significance for understanding the early history of the universe, and enriching the element nucleosynthesis theory. Based on the observed abundances of weak r-process star HD 140283 and theoretical yields of single supernova (SN), we fit the observational elemental abundances (from O to Zn) to the entire library of single SN yield, and derive that HD 140283 may have been born from a nebula polluted by the explosion of supernova whose progenitor mass is 22.5 M⊙(the subscript \⊙" means the solar mass). Based on the same method, we study the other ve typical weak r-process stars, and respectively derive the progenitor masses of supernova which have polluted the nebulas forming these stars. Furthermore, the possible astrophysics sources of weak r-process are inferred.

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马文娟,李宏杰,张璐,张波. HD 140283元素丰度分析及弱r-过程元素天体物理来源[J].天文学报,2020,(5):1-7.

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  • 收稿日期:2019-11-17
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  • 在线发布日期: 2020-09-29
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