The First Chemical Enrichment in the Universe and the Formation of Hyper Metal-Poor Stars
The First Chemical Enrichment in the Universe and the Formation of Hyper Metal-Poor Stars
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DOI：
10.1126/science.1112997
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发表时间：
2005-05
期刊：
影响因子：
56.9
通讯作者：
N. Iwamoto;H. Umeda;N. Tominaga;K. Nomoto;K. Maeda
中科院分区：
文献类型：
--
作者：
N. Iwamoto;H. Umeda;N. Tominaga;K. Nomoto;K. Maeda
最近发现的一颗金属丰度Fe/H小于太阳的十万分之一的超贫金属（HMP）恒星，以及一颗早期的HMP恒星，提出了一个具有挑战性的问题，即这些HMP恒星是否是宇宙中真正的第一代低质量恒星。我们认为，这些HMP恒星是由第一代超新星的化学富集气体形成的第二代恒星。这个解决方案的关键是这些HMP恒星非常不寻常的丰度模式以及它们之间的相似性和差异性。我们可以用核心坍缩的“微弱”超新星模型重现这些丰度特征，其中包括爆炸期间广泛的物质混合和回落。
The recent discovery of a hyper–metal-poor (HMP) star, with a metallicity Fe/H smaller than 1/100,000 of the solar ratio, together with one earlier HMP star, has raised a challenging question whether these HMP stars are the actual first-generation, low-mass stars of the universe. We argue that these HMP stars are second-generation stars formed from gases that were chemically enriched by the first-generation supernovae. The key to this solution is the very unusual abundance patterns of these HMP stars and the similarities and differences between them. We can reproduce these abundance features with core-collapse “faint” supernova models that include extensive matter mixing and fallback during explosions.