Abstract
Recent surveys of metal-deficient stars have discovered a large number of carbon-rich objects, with a marked increase in their frequency at [Fe/H] < −2.5. In order to constrain the origin(s) of their carbon excesses, we have performed elemental abundance analyses for 40 objects selected from candidate metal-poor stars with strong CH Gbands identified in the HK and Hamburg/ESO surveys. High-resolution spectroscopy has beenobtained with AAT/UCLES and Subaru/HDS; a portion of these studies have already been published [1–3].
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Aoki, W. et al. (2006). The Chemical Compositions of Carbon-Enhanced Metal-Poor Stars. In: Randich, S., Pasquini, L. (eds) Chemical Abundances and Mixing in Stars in the Milky Way and its Satellites. ESO ASTROPHYSICS SYMPOSIA. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-34136-9_44
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DOI: https://doi.org/10.1007/978-3-540-34136-9_44
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