Astronomy and Astrophysics – Astronomy
Scientific paper
May 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985aj.....90..803r&link_type=abstract
Astronomical Journal (ISSN 0004-6256), vol. 90, May 1985, p. 803-811.
Astronomy and Astrophysics
Astronomy
22
Dwarf Stars, G Stars, Galactic Structure, Main Sequence Stars, Metallic Stars, Milky Way Galaxy, Stellar Spectra, Color-Magnitude Diagram, Giant Stars, Stellar Luminosity, Stellar Magnitude
Scientific paper
Using a quantitative, three-dimensional spectral classification system developed earlier (Rose 1984), a class of strong lined dwarf stars has been identified in the Galactic disk. The strong-lined dwarfs were found in a sample of G5-G7 stars with m(B) of about 11 classified as giants by Upgren (1962) in his North Galactic Pole survey. The misclassification in luminosity on Upgren objective-prism spectra results from the great strength of the CN bands in these stars. The strong-lined stars are determined to be dwarfs from a measurement of the strength of Sr II 4077 A relative to neighboring Fe I lines. Furthermore, these stars are found to be strong lined in Fe and to have anomalous broadband colors that suggest heavy line blanketing. They have properties similar to stars with Fe/H abundance ratios + 0.25 in the Cayrel de Strobel and Bentolila (1983) Fe/H abundance catalog. The strong lined dwarfs contribute about 25 percent of the G5-G7 dwarfs at m(B) of about 11 in the Upgren survey. However, there is a selection bias in favor of the strong-lined dwarfs, since they are hotter, and hence more luminous, than solar-abundance dwarfs of the same spectral type. When this selection effect is accounted for, it is found that the strong lined stars comprise about 15 percent of the Galactic disk.
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