Astron. Astrophys. 353, 978-986 (2000)

Oxygen abundance in halo stars from O I triplet

T.V. Mishenina ¹, S.A. Korotin ¹, V.G. Klochkova ² and V.E. Panchuk <sup>2

1</sup> Department of Astronomy, Odessa State University, Shevchenko Park, 270014 Odessa, Ukraine (skyline@eurocom.od.ua; tamar@deneb.odessa.ua)
² Special Astrophysical Observatory of the Russian AS, 357147 Nizhnij Arkhyz, Russia (valenta@sao.ru)

Received 2 June 1999 / Accepted 10 September 1999

Abstract

Oxygen abundance for 14 halo stars through the O I 7774 Å triplet have been derived from high resolution spectra ( ) obtained with echelle-spectrometer of 6-m telescope of Special Astrophysical Observatory of the Russian Academy of Sciences. The effective temperature, metallicity and other parameters have been examined. For example, the effective temperature was found from line wings and photometric indices. The abundance analysis was carried out using both LTE and non-LTE conceptions. For this aim, we have specified the oxygen atomic model.

The average [O/Fe] value appeared to be from the non-LTE determination. A trend of oxygen abundance increasing along with the iron abundance decreasing was found. The relation between [O/Fe] and [Fe/H] is linear: . In addition to the sample of our program stars, we also involved in the analysis, 24 targets from Cavallo et al. (1997). For their original results we have determined the necessary non-LTE corrections.

Our data are compared with the results of other works (Tomkin et al., 1992; King & Boesgaard, 1995; Boesgaard et al. 1999).

Key words: atomic processes line: formation line: profiles methods: numerical stars: abundances stars: atmospheres

Send offprint requests to: S.A. Korotin

© European Southern Observatory (ESO) 2000

Online publication: January 18, 2000

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