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NLTE Masking and the Kiev Fe I Oscillator Strengths

Published online by Cambridge University Press:  30 March 2016

Robert J. Rutten
Robert J. Rutten*
Affiliation:
Sterrewacht Sonnenborgh, Zonnenburg 2, 3512 NL UTRECHT, The Netherlands

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This contribution serves to advertise the empirical solar-spectrum determinations of the oscillator strengths of 860 Fe I lines by Gurtovenko and Kostik (1981), by showing that these Kiev data contain just the lines needed in cool-star abundance analyses, and by explaining why they are so good. For details, see Rutten and Kostik (1982) and Rutten and Zwaan (1983).

Figures 1 and 2 show why the Kiev gf-values are so useful. While the precise Oxford measurements (see Simmons and Blackwell, 1982, for references) cover the low-excitation lines (Fig. la) which are mostly too violet and too strong for abundance studies, the Kiev workers have added the best lines in the solar visual, thus precisely the weaker lines of higher excitation one needs (Fig. 1b). Figure 2 demonstrates this for the solar Fe I curve of growth: the Doppler part, which is the only really useful part, is made up of Kiev lines (dots).

Type
Joint Commission Meetings
Information
Highlights of Astronomy , Volume 6: Highlights of Astronomy. As presented at the XVIIIth General Assembly of the IAU, 1982 , 1983 , pp. 801 - 803
Copyright
Copyright © Reidel 1983

References

Gingerlch, O., Noyes, R.W., Kalkofen, W., and Cuny, Y.: 1971, Solar Phys. 18, p. 347 (HSRA).Google Scholar
Gurtovenko, E.A. and Kostlk, R.I.: 1981, Astron. and Ap. Suppl. 46, p. 239.Google Scholar
Holweger, H. and Müller, E.A.: 1974, Solar Phys. 9, p. 19 (HOLMUL).Google Scholar
Lites, B.W.: 1972, NCAR Cooperative Thesis No. 28, Univ. of Colorado and High Altitude Observatory, NCAR, Boulder.Google Scholar
Rutten, R.J. and Kostlk, R.I.: 1982, Astron. and Ap., in press; preprint available.Google Scholar
Rutten, R.J. and Zwaan, C.: 1983, Astron. and Ap., in press, preprint available.Google Scholar
Simmons, G.J. and Blackwell, D.E.: 1982, Astron. and Ap. 112, p. 209.Google Scholar