Relative abundances in metal-poor stars. II - The carbon-to-iron ratio

Details Relative abundances in metal-poor stars. II - The carbon-to-iron ratio Relative abundances in metal-poor stars. II - The carbon-to-iron ratio

Nov 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...225..913p&link_type=abstract

Astrophysical Journal, Part 1, vol. 225, Nov. 1, 1978, p. 913-918.

Statistics

Computation

38

Abundance, Carbon, Dwarf Stars, Iron, Stellar Atmospheres, Stellar Models, Galactic Evolution, Hydrogen Atoms, Metals, Spectrum Analysis

Scientific paper

The abundance of carbon has been determined (or an upper limit established) by spectral synthesis of CH features in a dozen field dwarfs and subgiants of metallicities 1/5 to 1/100 solar. All program stars were selected from the Eggen high-velocity catalog, observed with the SAO echelle-Kron system at Mount Hopkins, Arizona, and analyzed by using model-atmosphere computations of broad-band colors and weak atomic lines. The CH features reveal that all these stars have essentially the solar carbon-to-iron ratio, given the plus or minus 0.2 dex uncertainty in the normalization to the solar value, and the plus or minus 0.14 dex uncertainty in an individual stellar carbon-abundance determination relative to others. Several implications of this uniformity for studies of the evolution of the Galaxy as a whole are briefly discussed.

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