Volume 430, Number 1, January IV 2005
|Page(s)||255 - 262|
|Section||Stellar structure and evolution|
|Published online||12 January 2005|
Astrophysical Research Center for the Structure and Evolution of the Cosmos (ARCSEC), Sejong University, Seoul 143-747, Korea e-mail: email@example.com; firstname.lastname@example.org
2 Odessa Astronomical observatory, Odessa National University, Park Shevchenko, Odessa 65014, Ukraine e-mail: email@example.com; firstname.lastname@example.org
3 Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, 1050 Brussels, Belgium e-mail: email@example.com
4 Special Astrophysical observatory of the Russian Academy of Sciences, Nizhnij Arkhyz, Zelenchuk, Karachaevo-Cherkesiya 369167, Russia e-mail: firstname.lastname@example.org
5 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 e-mail: email@example.com
6 Shamakhy Astrophysical Observatory, NAS of Azerbaijan, Yusif Mamedaliev, Shamakhy, Azerbaijan
7 Main Astronomical observatory, NAS of Ukraine, Kiiv 03680, Ukraine e-mail: firstname.lastname@example.org
8 Department of Earth Science Education, Chonbuk National University, Chonju 561-756, Korea e-mail: email@example.com
9 Odessa National University, Odessa 65014, Ukraine e-mail: firstname.lastname@example.org
Accepted: 8 September 2004
We report the abundance determination in the atmosphere of the bright halo star HD 221170. The spectra were taken with the Terskol Observatory's 2.0-m telescope with a resolution 45 000 and signal-to-noise ratio up to 250 in the wavelength region 3638–10 275 Å. The adopted atmospheric parameters correspond to an effective temperature = 4475 K, a surface gravity = 1.0, a microturbulent velocity = 1.7 , and a macroturbulent velocity = 4 . The abundances of 43 chemical elements were determined with the method of spectrum synthesis. The large overabundances (by 1 dex relative to iron) of elements with Z > 38 are shown to follow the same pattern as the solar r-abundances. The present HD 221170 analysis confirms the non-universality of the r-process, or more exactly the observation that the astrophysical sites hosting the r-process do not always lead to a unique relative abundance distribution for the bulk Ba to Hg elements, the Pb-peak elements, and the actinides.
Key words: line: identification / stars: abundances / stars: atmospheres / stars: evolution / stars: individual: HD 221170 / nuclear reactions, nucleosynthesis, abundances
© ESO, 2005
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