Volume 423, Number 2, August IV 2004
|Page(s)||683 - 691|
|Published online||06 August 2004|
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR China e-mail: email@example.com
2 Institut für Astronomie und Astrophysik der Universität München, Scheinerstrasse 1, 81679 München, Germany
Accepted: 4 May 2004
We present sodium abundances for a sample of nearby stars. All results have been derived from NLTE statistical equilibrium calculations. The influence of collisional interactions with electrons and hydrogen atoms is evaluated by comparison of the solar spectrum with very precise fits to the line cores. The NLTE effects are more pronounced in metal-poor stars since the statistical equilibrium is dominated by collisions of which at least the electronic component is substantially reduced. The resulting influence on the determination of sodium abundances is in a direction opposite to that found previously for Mg and Al. The NLTE corrections are about -0.1 in thick-disk stars with . Our [Na/Fe] abundance ratios are about solar for thick- and thin-disk stars. The increase in [Na/Fe] as a function of [Fe/H] for metal-rich stars found by Edvardsson et al. ([CITE]) is confirmed. Our results suggest that sodium yields increase with the metallicity, and quite large amounts of sodium may be produced by AGB stars. We find that [Na/Fe] ratios, together with either [Mg/Fe] ratio, kinematic data or stellar evolutionary ages, make possible the individual discrimination between thin- and thick-disk membership.
Key words: line: formation / line: profiles / stars: abundances / stars: late-type / Galaxy: evolution
© ESO, 2004
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