Volume 413, Number 3, January III 2004
|Page(s)||1105 - 1114|
|Published online||07 January 2004|
The chemical composition of the mild barium star HD 202109*
Odessa Astronomical observatory, Odessa National University, Park Shevchenko, Odessa 65014, Ukraine e-mail: email@example.com,firstname.lastname@example.org
2 Isaac Newton Institute, Santiago, Chile, Odessa branch, Ukraine
3 Department of Earth Science Education, Chonbuk National University, Chonju 561-756, Korea e-mail: email@example.com
4 National Astronomical Observatories, Chinese Academy of Sciences, 100012 Beijing, PR China
5 GEPI, Observatoire de Paris-Meudon, 92195 Meudon, France
6 Institut für Astronomie und Astrophysik der Universität München, Universitäts-Sternwarte München, Scheinerstr. 1, 81679 München, Germany
7 The International Centre for Astronomical, Medical and Ecological Research of the Russian Academy of Sciences and the National Academy of Sciences of Ukraine, Golosiiv, Kiev 03680, Ukraine (ICAMER) e-mail: firstname.lastname@example.org
8 Special Astrophysical observatory of the Russian Academy of Sciences, Nizhnij Arkhyz, Zelenchuk, Karachaevo-Cherkesiya 369167, Russia e-mail: email@example.com,firstname.lastname@example.org
9 Isaac Newton Institute, Santiago, Chile, SAO branch, Russia
Corresponding author: A. V. Yushchenko, email@example.com
Accepted: 7 August 2003
We present chemical abundances of the mild barium star HD 202109 (ζ Cyg) determined from the analysis of a spectrum obtained by using the 2-m telescope at the Peak Terskol Observatory and a high-resolution spectrometer with , signal to noise ratio >100. We also present the atmospheric parameters of the star determined using various methods including iron-line abundance analysis. For line identifications, we use whole-range synthetic spectra computed from Kurucz's database and the latest lists of spectral lines. Among the determined abundances of 51 elements, those of P, S, K, Cu, Zn, Ge, Rb, Sr, Nb, Mo, Ru, Rh, Pd, In, Sm, Gd, Tb, Dy, Er, Tm, Hf, Os, Ir, Pt, Tl, and Pb were not investigated previously. Assuming that the overabundance pattern of Ba stars is due to binary accretion, the observed abundance pattern of the neutron-capture process elements in HD 202109 can be explained by combining the AGB star nucleosynthesis and the wind accretion scenario.
Key words: line: identification / stars: abundances / stars: atmospheres / stars: evolution / stars: binaries / stars: individual: HD 202109
© ESO, 2004
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