The metallicity and UV excesses of late main-sequence stars

Details The metallicity and UV excesses of late main-sequence stars The metallicity and UV excesses of late main-sequence stars

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987azh....64..586s&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 64, May-June 1987, p. 586-590. In Russian.

Astronomy and Astrophysics

Astronomy

Late Stars, Main Sequence Stars, Metallicity, Stellar Composition, Ultraviolet Spectra, F Stars, G Stars, Hydrogen, Iron, K Stars, Star Clusters, Ubv Spectra

Scientific paper

A comparison of the characteristics of the distributions of delta (U-B) (UV excesses) and the concentration of Fe/H (metallicity) of F, G, and K dwarfs reveals a number of discrepancies. These can be eliminated by assuming that the UV excesses of K and late G dwarfs and the Fe/H concentration values of F dwarfs are too low. In effect, the F5-F9 dwarfs turn out to be more metal-rich than G and K dwarfs and the metallicity of the Hyades cluster, relative to the sun, turns out to be + 0.1.

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