Original article can be found at: http://www.aanda.org/--Copyright The European Southern Observatory (ESO) DOI : 10.1051/0004-6361:20053182Peer reviewe

Garcia Perez, A.E.

Primas, F.

Astronomy and Astrophysics

English

arXiv

A. E. García Pérez

F. Primas

Crossref

Li and Be depletion in metal-poor subgiants

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.</p

García Pérez, Ana Elia,

Primas, Francesca

Swepub

University of Hertfordshire Research Archive

336: Cosmic Abundances as Records of Stellar Evolution

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 $\ion{Li}{i}$ line (670.78 nm) and
100 for the $\ion{Be}{ii}$ doublet lines (313.04 nm). The spectral
analysis of the observations was carried out using the Uppsala suite of
 codes and marc

EDP Sciences OAI-PMH repository (1.2.0)

https://www.aanda.org/articles/aa/pdf/2006/07/aa3182-05.pdf

Li and Be depletion in metal-poor subgiants

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University of Hertfordshire Research Archive

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