Statistics – Computation
Scientific paper
Mar 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990pazh...16..213b&link_type=abstract
Pis'ma v Astronomicheskii Zhurnal (ISSN 0320-0108), vol. 16, March 1990, p. 213-222. In Russian. In Russian. In Russian.
Statistics
Computation
1
Abundance, Metal Ions, Metallicity, Stellar Atmospheres, Stellar Spectra, Subdwarf Stars, Atmospheric Models, Iron, Line Spectra, Spectrographs
Scientific paper
The model atmosphere method is used to perform iron abundance computations for 30 subdwarfs with T(eff) between 5500 and 6500 K in the Fe/H range between -0.1 and -2.3. It is shown that there is a systematic difference in the iron abundances determined from Fe I and Fe II lines. This difference increases with decreasing metallicity. Non-LTE computations of the Fe I-Fe II ionization balance are performed using observed UV fluxes. It is found that, in the atmospheres of subdwarfs, an overionization of neutral iron atoms occurs, leading to a weakening of Fe I line intensity and to the systematic underestimation of the abundances. It is concluded that the Fe II lines must be used for correct determinations of iron abundance in the atmospheres of subdwarfs since they are not sensitive to the effect of the overionization of Fe I.
Bikmaev I. F.
Bobritskij S. S.
Sakhibullin N. A.
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