First Stars II. Elemental abundances in the extremely metal-poor star CS 22949–037
نویسندگان
چکیده
منابع مشابه
Abundances of Extremely Metal-Poor Star Candidates
We present chemical abundances for 110 stars identified in objective-prism surveys as candidates to be very metal-poor. The abundances are derived from high S/N, intermediate-resolution spectra obtained with the Keck Observatory Echelle Spectrometer and Imager. An additional 25 stars with well-determined abundances ranging from [Fe/H]= −1.5 and −3.2 were observed and the results used to help ca...
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We have determined Li abundances for eleven metal-poor turn-off stars, among which eight have [Fe/H] < −3, based on LTE analyses of high-resolution spectra obtained with the HDS on the Subaru telescope. The Li abundances for four of these eight stars are determined for the first time by this study. Effective temperatures are determined by a profile analysis of Hα and Hβ. While seven stars have ...
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We present a high-resolution spectroscopic analysis of the extremely-metal-poor star CS 22957-027, which Beers et al. (1992) noted to exhibit a rather strong G-band. For T eff = 4839 K, derived from broadband photometry, our analysis obtains log g= 2.25, and a very low metallicity of [Fe/H]=−3.43 ± 0.12. The carbon-to-iron ratio is found to be enhanced by ≈ 2 dex relative to the solar value, si...
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We present oxygen abundances derived from both the permitted and forbidden oxygen lines for 55 subgiants and giants with [Fe/H] values between −2.7 and solar with the goal of understanding the discrepancy in the derived abundances. A first attempt, using Teff values from photometric calibrations and surface gravities from luminosities, obtained agreement between the indicators for turn-off star...
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We have determined beryllium abundances for 25 metal-poor stars based on the high resolution and high signal-to-noise ratio spectra from the VLT/UVES database. Our results confirm that Be abundances increase with Fe, supporting the global enrichment of Be in the Galaxy. Oxygen abundances based on [O i] forbidden line implies a linear relation with a slope close to one for the Be vs. O trend, wh...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2002
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20020687