Other
Scientific paper
Nov 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...322..930t&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 322, Nov. 15, 1987, p. 930-948.
Other
19
Late Stars, Metallic Stars, Molecular Spectra, Spectral Bands, Stellar Composition, Stellar Spectra, Data Bases, Dwarf Stars, Spectrum Analysis, Stellar Atmospheres, Stellar Evolution
Scientific paper
This paper considers absorption features in nearby, very strong lined (VSL) G and K stars. These are the stars which traditionally have been called "super-metal-rich" (SMR). The data include measurements made by Spinrad and Taylor, more recent data of the same kind, and a temperature index (Cousins R - I). The other indices adopted measure narrow-band blanketing, broad-band blanketing, and strong absorption features of CN, Ca I, CH, Mg I, and Na I. For dwarfs, data for Fe I and Ca II are also analyzed. It is found that with two exceptions (CH in giants, Ca II in dwarfs), G and K VSL stars have enhancements in all these features. For disk G and K stars in general, there is a positive correlation between the temperature-corrected strengths of most indices. A feature is enhanced in VSL stars if and only if it participates in this correlation. The VSL stars are therefore simply strong-featured examples of disk stars. For non-VSL stars, stronger (weaker) features are associated with higher (lower) overall metallicities. If this correlation applies also to VSL stars, they are super-metal-rich. The authors discuss possibilities which might explain the VSL enhancements without appeal to supermetallicity. None of these "Alternatives X" are clearly satisfactory, but the existence for an Alternative X is not ruled out.
Johnson Scott B.
Taylor Benjamin J.
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