Spectroscopic analysis of extreme metal-poor 'dwarfs'. I Observational material, Fe lines, and model atmospheres

Details Spectroscopic analysis of extreme metal-poor 'dwarfs'. I Observational material, Fe lines, and model atmospheres Spectroscopic analysis of extreme metal-poor 'dwarfs'. I Observational material, Fe lines, and model atmospheres

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...132..208m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 132, no. 1, March 1984, p. 208-218.

Astronomy and Astrophysics

Astrophysics

31

Abundance, Dwarf Stars, Metallicity, Spectroscopic Analysis, Stellar Spectra, Gravitation, Iron, Late Stars, Stellar Temperature, Surfaces

Scientific paper

Fe lines are analysed in the spectra of the two extreme metal-poor stars MD 19445 and MD 140283 on the basis of new observational material. It is shown that the use of accurate equivalent widths and very accurate oscillator strengths improves significantly the quality of the analysis. In particular, these stars are found to be more metal-deficient than precedingly thought. This result may imply a significant revision of the adopted abundance scale. It is shown that differential analyses of such stars relative to the Sun are subject to important systematic errors due to the very large difference between the stellar and solar equivalent widths. Finally, the temperature criteria are analysed and it is argued that the criteria linked to deep atmospheric layers, such as the B - V colour or the hydrogen line wings, should not be used to select a model representing satisfactorily the line-forming layers.

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