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

F. Primas; M. Asplund; P. E. Nissen; V. Hill

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

F. Primas·M. Asplund·P. E. Nissen·V. Hill

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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 Be content. The spectra were observed during the Science Verification of UVES, the ESO VLT Ultraviolet and Visible Echelle Spectrograph. The high resolution (~48,000) and high S/N (~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 +/- 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.

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F. Primas, M. Asplund, P. E. Nissen, V. Hill. 2000-09-29. The beryllium abundance in the very metal-poor halo star G 64-12 from VLT/UVES observations. https://arxiv.org/abs/astro-ph/0009482

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