Journal
SCIENCE
Volume 309, Issue 5733, Pages 451-453Publisher
AMER ASSOC ADVANCEMENT SCIENCE
DOI: 10.1126/science.1112997
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The recent discovery of a hyper-metal-poor (HMP) star, with a metalticity Fe/H smaller than 1/1000,000 of the solar ratio, together with one earlier HMP star, has raised a challenging question whether these HMP stars are the actual first-generation, tow-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.
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