Atmospheric chemical composition of the halo star HD 221170 from a synthetic-spectrum analysis |
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| Authors: | V F Gopka A V Yushchenko T V Mishenina Chulhee Kim F A Musaev A V Bondar’ |
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| Institution: | (1) Odessa Astronomical Observatory, Mechnikov Odessa National University, Park Shevchenko, Odessa, 65014, Ukraine;(2) Chungbuk National University, Chungju, 361-763, Korea;(3) Chonbuk National University, Chonju, 561-756, Korea;(4) Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz, Karachai-Cherkesian Republic, 369167, Russia;(5) International Center for Astronomical and Medical-Biological Research of National Academy of Sciences of Ukraine and Russian Academy of Sciences, Golosiiv, Kiev, 03680, Ukraine |
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| Abstract: | The atmospheric abundances of 30 chemical elements in the halo star HD 221170 are analyzed by fitting synthetic spectra to observed spectra (i) with a resolution of 60 000 and signal-to-noise ratios of about 200 taken with the 1.93-m telescope of the Observatoire de Haute Provence and (ii) with a resolution of 35 000 and signal-to-noise ratios of more than 100 taken with the 2-m telescope of the Terskol Peak Observatory. The derived parameters of the stellar atmosphere are Teff=4475 K, log g=1.0, Fe/H]=?2.03, Vmicro=1.7 km/s, and Vmacro=4 km/s. The parameters Teff, log g, Fe/H], and Vmicro can be determined by analyzing the variations of the rms error of the mean iron abundance derived using different model atmospheres. The chemical composition of the star’s atmosphere is analyzed. The abundances of a total of 35 elements in HD 221170 have been derived in this paper and in previous studies. Overall, the abundances of elements lighter than praseodymium are consistent with the elemental abundances in the atmospheres of stars with similar metal deficits. Copper and manganese are underabundant by ?2.9 and ?2.6 dex, respectively, relative to the Sun (when the analysis includes the effects of hyperfine structure). Heavy r-process elements (starting from praseodymium) are overabundant compared to iron-group elements. This can be explained by an enrichment in r-process elements of the material from which the star was formed. |
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