The iron abundance in the Hyades Cluster

Details The iron abundance in the Hyades Cluster The iron abundance in the Hyades Cluster

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...241l..83b&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 241, Oct. 15, 1980, p. L83-L87. Research supported by the Robert A.

Astronomy and Astrophysics

Astrophysics

56

Abundance, Iron, Metallic Stars, Star Clusters, Stellar Spectrophotometry, Dwarf Stars, G Stars, H Alpha Line, Solar Atmosphere, Spectral Line Width, Stellar Atmospheres, Stellar Luminosity, Stellar Temperature

Scientific paper

Low-noise Reticon spectra of the moon and two Hyades G dwarfs are used to derive the metallicity of the Hyades Cluster. The relative temperatures of the sun and the Hyades stars are determined from the wings of their H-alpha profiles, and iron abundances are based on weak Fe I lines. The spectroscopic result is an Fe/H ratio of 0.20 + or - 0.1, in good agreement with photometric determinations of the Hyades metallicity. The B-V color of the sun is inferred to be 0.64 + or 0.02.

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