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Astron. Astrophys. 364, L42-L46 (2000)

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Letter to the Editor

The beryllium abundance in the very metal-poor halo star G 64-12 from VLT/UVES observations *

F. Primas  **  1, M. Asplund 2, P.E. Nissen 3 and V. Hill 1

1 European Southern Observatory, Karl-Schwarzschild Strasse 2, 85748 Garching bei München (fprimas@eso.org, vhill@eso.org)
2 Uppsala Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden (martin@astro.uu.se)
3 Aarhus University, Institute of Physics and Astronomy, Denmark (pen@ifa.au.dk)

Received 16 August 2000 / Accepted 28 August 2000

Abstract

We report on a new spectroscopic analysis of the very metal deficient star G 64-12 ([Fe/H]=-3.3), aimed at determining, for the first time, its beryllium content. The spectra were observed during the Science Verification of UVES, the ESO VLT Ultraviolet and Visible Echelle Spectrograph. The high resolution ([FORMULA]48 000) and high S/N ([FORMULA]130 per pixel) achieved at the wavelengths of the BeII resonance doublet allowed an accurate determination of its abundance: log N(Be/H) = -13.10 [FORMULA] 0.15 dex. The Be abundance is significantly higher than expected from previous measurements of Be in stars of similar metallicity (3D and NLTE corrections acting to make a slightly higher value than an LTE analysis). When compared to iron, the high [Be/Fe] ratio thus found may suggest a flattening in the beryllium evolutionary trend at the lowest metallicity end or the presence of dispersion at early epochs of galactic evolution.

Key words: Stars: Population II, abundances, atmospheres – - Galaxy: halo – - Instrumentation: spectrographs

* Based on observations taken during the Science Verification of UVES at the VLT/Kueyen telescope, European Southern Observatory, Paranal, Chile
** Visiting Researcher (CNRS) at the Laboratoire d'Astrophysique - Observatoire de Midi-Pyrénées, Toulouse, France

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© European Southern Observatory (ESO) 2000

Online publication: December 15, 2000
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