Volume 389, Number 2, July II 2002
|Page(s)||537 - 546|
|Section||Stellar structure and evolution|
|Published online||27 June 2002|
Department of Astronomy, Kazan State University, Kremlevskaya 18, 420008 Kazan, Russia e-mail: Ilfan.Bikmaev@ksu.ru
2 Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya 48, 109017 Moscow, Russia
3 Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria e-mail: email@example.com
4 Institute for Physics and Astronomy, University of Aarhus, Bygn. 520, 8000 Aarhus C, Denmark e-mail: firstname.lastname@example.org
5 Special Astrophysical Observatory RAS, 369167 Nizhnij Arkhyz, Karachai-Circassian Republic, Russia e-mail: email@example.com
6 SAO Branch of Isaac Newton Institute, Santiago, Chile
7 International Centre for Astronomical, Medical and Ecological Researches (ICAMER), National Academy of Sciences of Ukraine, 361605 Peak Terskol, Kabardino-Balkaria, Russia
8 Department of Astronomy and Space Physics, Uppsala University, Box 515, 751-20 Uppsala, Sweden e-mail: firstname.lastname@example.org
Corresponding author: T. Ryabchikova, email@example.com
Accepted: 9 April 2002
We have performed abundance analysis of two slowly rotating, late A-type stars, HD 32115 (HR 1613) and HD 37594 (HR 1940), based on obtained echelle spectra covering the spectral range 4000–9850 Å. These spectra allowed us to identify an extensive line list for 31 chemical elements, the most complete to date for A-type stars. Two approaches to abundance analysis were used, namely a “manual” (interactive) and a semi-automatic procedure for comparison of synthetic and observed spectra and equivalent widths. For some elements non-LTE (NLTE) calculations were carried out and the corresponding corrections have been applied. The abundance pattern of HD 32115 was found to be very close to the solar abundance pattern, and thus may be used as an abundance standard for chemical composition studies in middle and late A stars. Further, its Hα line profile shows no core-to-wing anomaly like that found for cool Ap stars and therefore also may be used as a standard in comparative studies of the atmospheric structures of cool, slowly rotating Ap stars. HD 37594 shows a metal deficiency at the level of -0.3 dex for most elements and triangle-like cores of spectral lines. This star most probably belongs to the δ Sct group.
Key words: stars: atmospheres / stars: abundances / stars: individual: HD 32115, HD 37594
© ESO, 2002
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