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Metal poor stars

  1. May 27, 2005 #1

    wolram

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    http://arxiv.org/PS_cache/astro-ph/pdf/0505/0505524.pdf

    Title: The first chemical enrichment in the universe and the formation of hyper metal-poor stars
    Authors: Nobuyuki Iwamoto, Hideyuki Umeda, Nozomu Tominaga, Ken'ichi Nomoto, Keiichi Maeda
    Comments: To be published in Science. 12 pages, 3 figures

    The recent discovery of a hyper metal-poor (HMP) star, whose metallicity Fe/H is smaller than 1/100,000 of the solar ratio, together with one earlier HMP star, has raised a challenging question if these HMP stars are the actual first generation, low mass stars in the Universe. We argue that these HMP stars are the second generation stars being formed from gases which were chemically enriched by the first generation supernovae. The key to this solution is the very unusual abundance patterns of these HMP stars with important similarities and differences. We can reproduce these abundance features with the core-collapse ``faint'' supernova models which undergo extensive matter mixing and fallback during the explosion.
     
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  3. May 27, 2005 #2

    wolram

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    Are these two stars pop 111? the chemical make up is suggestive that they
    are, the close binary idea seems less likely to me.
     
  4. May 27, 2005 #3

    SpaceTiger

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    Isn't that the opposite of the conclusion reached by the paper? Do you not agree with their findings?
     
  5. May 27, 2005 #4

    wolram

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    Space Tiger

    Isn't that the opposite of the conclusion reached by the paper? Do you not agree with their findings?

    Im not sure what their findings are, it always seems that more than one
    possibility exists, and the most intuitive is always the one that is over ridden?
     
  6. May 27, 2005 #5

    SpaceTiger

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    It says in the abstract you posted. They find that the abundances are consistent with supernova enrichment (i.e. not Pop III).
     
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