Abundance analyses of metal-poor stars. II - Yellow spectra of five dwarfs

Details Abundance analyses of metal-poor stars. II - Yellow spectra of five dwarfs Abundance analyses of metal-poor stars. II - Yellow spectra of five dwarfs

Aug 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...231..762p&link_type=abstract

Astrophysical Journal, Part 1, vol. 231, Aug. 1, 1979, p. 762-780. Research supported by Harvard University

Astronomy and Astrophysics

Astrophysics

97

Abundance, Dwarf Stars, Line Spectra, Metals, Ultraviolet Spectra, High Resolution, Iron, Solar Flux, Solar Spectra, Stellar Models, Stellar Spectrophotometry, Stellar Temperature, Subdwarf Stars, Tables (Data)

Scientific paper

The paper is the second in a series aimed at determining elemental abundances in metal-poor stars. It describes in detail several aspects important to the accuracy of the analysis of moderately and extremely metal-poor dwarfs of temperatures in the range 6200-5000 K. Five high-velocity metal-poor dwarfs - HD 84937, HD 103095, HD 114762, HD 132142, and HD 140283 - are analyzed. A procedure is presented for converting the photoelectrical spectra into intensity versus wavelength information. The use of a relationship between equivalent width divided by wavelength and central residual intensity to measure equivalent width is examined, where width errors are also evaluated. Various arguments are presented that the arc gf-values, the most extensive and widely used set of Fe I measurements available, contain systematic errors which depend on both the excitation level and the strength of a given transition. This possibility greatly limits the number of Fe I lines that can be reliably used to determine iron abundances in extremely weak-lined stars. Pertinent graphs and tables are included.

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