[KSCI] Korea Science Citation Index Service

http://dx.doi.org/10.5303/JKAS.2002.35.4.209

CHEMICAL ABUNDANCE PATTERNS FOR SHARP-LINED STARS

YUSHCHENKO ALEXANDER (Chonbuk National University, Odessa Astronomical observatory (OAO), Odessa National University)
GOPKA VERA (Odessa Astronomical observatory (OAO), Odessa National University)
KIM CHULHEE (Chonbuk National University)
KHOKHLOVA VERA (Institute of Astronomy of the Russian Academy of Sciences (RAS))
SHAYRINA ANGELINA (Main Astronomical observatory (NASU))
MUSAEV FAIG (The International Centre for Astronomical, Medical and Ecological Research of RAS and the National Academy of Sciences of Ukraine (NASU) - ICAMER, Special Astrophysical Observatory (RAS))
GALAZUTDINOV GAZINUR (The International Centre for Astronomical, Medical and Ecological Research of RAS and the National Academy of Sciences of Ukraine (NASU) - ICAMER, Special Astrophysical Observatory (RAS))
PAYLENKO YAKOY (Main Astronomical observatory (NASU))
MISHENINA TAMARA (Odessa Astronomical observatory (OAO), Odessa National University)
POLOSUKHINA NINA (Crimean Astrophysical Observatory)
NORTH PITER (Inst. d'Astronomie)

Publication Information

Journal of The Korean Astronomical Society / v.35, no.4, 2002 , pp. 209-220 More about this Journal

Abstract

In order to increase the completeness of the investigations of stellar abundances, we can use spectrum synthesis method, new atomic data and observation of stellar spectra with resolution comparable to solar spectral atlases. We made a brief review of main problems of these three ways. We present new results of abundance determinations in the atmospheres of four stars. The first is the implementation of new atomic data to well known Przybylski's star. We show that the number of spectral lines, which can be identificated in the spectrum of this star, can be significantly higher. The second example is the investigation of $\zeta$ Cyg. We found the abundances of 51 elements in the atmosphere of this mild barium star. The third example is halo star HD221170. Our preliminary abundance pattern consists of 42 elements. The heaviest elements in this pattern are U and Th. The last star is the spectroscopic binary HD153720. The number of elements investigated in the spectra of components of this star is not large, but the results show that the components are Am-stars.

Keywords

Line: identification; Stars: abundances; Stars: individual; HD101065; HD153720; HD202109; HD221170;

Citations & Related Records

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