Volume 447, Number 1, February III 2006
|Page(s)||299 - 310|
|Published online||27 January 2006|
Li and Be depletion in metal-poor subgiants
Department of Astronomy and Space Physics, Uppsala University, Box 515, 751 20 Uppsala, Sweden e-mail: email@example.com; A.E.Garcia-Perez@open.ac.uk
2 European Southern Observatory, Karl-Schwarzschild Strasse 2, 85748 Garching bei München, Germany e-mail: firstname.lastname@example.org
Accepted: 7 October 2005
A sample of metal-poor subgiants has been observed with the UVES spectrograph at the Very Large Telescope and abundances of Li and Be have been determined. Typical signal-to-noise per spectral bin values for the co-added spectra are of the order of 500 for the line (670.78 nm) and 100 for the doublet lines (313.04 nm). The spectral analysis of the observations was carried out using the Uppsala suite of codes and marcs (1D-LTE) model atmospheres with stellar parameters from photometry, parallaxes, isochrones and Fe ii lines. Abundance estimates of the light elements were corrected for departures from local thermodynamic equilibrium in the line formation. Effective temperatures and Li abundances seem to be correlated and Be abundances correlate with [O/H]. Standard models predict Li and Be abundances approximately one order of magnitude lower than main-sequence values which is in general agreement with the observations. On average, our observed depletions seem to be 0.1 dex smaller and between 0.2 and 0.4 dex larger (depending on which reference is taken) than those predicted for Li and Be, respectively. This is not surprising since the initial Li abundance, as derived from main-sequence stars on the Spite plateau, may be systematically in error by 0.1 dex or more, and uncertainties in the spectrum normalisation and continuum drawing may affect our Be abundances systematically.
Key words: stars: abundances / stars: atmospheres / stars: late type / stars: Population II
© ESO, 2006
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