Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5333
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dc.contributor.authorSbordone, L-
dc.contributor.authorBonifacio, P-
dc.contributor.authorCaffau, E-
dc.contributor.authorLudwig, H. -G-
dc.contributor.authorBehara, N-
dc.contributor.authorGonzalez-Hernandez, J. I-
dc.contributor.authorSteffen, M-
dc.contributor.authorCayrel, R-
dc.contributor.authorFreytag, B-
dc.contributor.authorVan't Veer, C-
dc.contributor.authorMolaro, P-
dc.contributor.authorPlez, B-
dc.contributor.authorSivarani, T-
dc.contributor.authorSpite, M-
dc.contributor.authorSpite, F-
dc.contributor.authorBeers, T. C-
dc.contributor.authorChristlieb, N-
dc.contributor.authorFrançois, P-
dc.contributor.authorHill, V-
dc.date.accessioned2011-02-02T10:38:25Z-
dc.date.available2011-02-02T10:38:25Z-
dc.date.issued2010-03-
dc.identifier.citationK. Cunha, M. Spite & B Barbuy, eds., Chemical abundances in the Universe: connecting first Stars to Planets, Proceedings IAU Symposium No. 265, 2009, pp. 75-76en
dc.identifier.urihttp://hdl.handle.net/2248/5333-
dc.descriptionRestricted Accessen
dc.description.abstractWe present the largest sample available to date of lithium abundances in extremely metal poor (EMP) Halo dwarfs. Four Teff estimators are used, including IRFM and Hα wings fitting against 3D hydrodynamical synthetic profiles. Lithium abundances are computed by means of 1D and 3D-hydrodynamical NLTE computations. Below [Fe/H]∼−3, a strong positive correlation of A(Li) with [Fe/H] appears, not influenced by the choice of the Teff estimator. A linear fit finds a slope of about 0.30 dex in A(Li) per dex in [Fe/H], significant to 2–3 σ, and consistent within 1 σ among all the Teff estimators. The scatter in A(Li) increases significantly below [Fe/H]∼–3. Above, the plateau lies at A(Li)3D,NLTE =2.199±0.086. If the primordial A(Li) is the one derived from standard Big Bang Nucleosynthesis (BBN), it appears difficult to envision a single depletion phenomenon producing a thin, metallicity independent plateau above [Fe/H]=−2.8, and a highly scattered, metallicity dependent distribution below.en
dc.language.isoenen
dc.publisherCambridge University Pressen
dc.relation.ispartofseriesIAU Symposium and Colloquium Proceedings Series; Vol. 265-
dc.relation.urihttp://dx.doi.org/10.1017/S1743921310000244en
dc.rights© Cambridge University Pressen
dc.subjectNuclear reactionsen
dc.subjectNucleosynthesisen
dc.subjectAbundances, Galaxyen
dc.subjectHalo, Galaxyen
dc.subjectAbundances, starsen
dc.subjectPopulation IIen
dc.titleThe metal–poor end of the Spite plateauen
dc.typeArticleen
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