S. Castro et al., HIGH-RESOLUTION ABUNDANCE ANALYSIS OF VERY METAL-RICH STARS IN THE SOLAR NEIGHBORHOOD, The Astronomical journal, 114(1), 1997, pp. 376-387
We report detailed analysis of high-resolution spectra of nine high ve
locity metal-rich dwarfs in the solar neighborhood, selected from the
proper motion samples of Grenon. The stars are super metal-rich, and 5
of them have [Fe/H]greater than or equal to+0.4, making them the most
metal-rich stars currently known, We find that alpha-elements decreas
e with increasing metallicity; s-elements are underabundant by about [
s-elements/Fe] approximate to-0.3; the Eu II line was measurable for 6
stars, showing [Eu/Fe]approximate to 0.0, except for G161-29 where [E
u/Fe]=+0.50, All calculations followed the same methods used by Castro
et al. [1996, AJ, 111, 2439] for the analysis of the well-known metal
-rich prototype mu Leo and the very strong-lined bulge star BW IV-167,
for which [Fe/H]=+0.36 and +0.17 were found, respectively. While exce
eding the [Fe/H] of current bulge samples, the chemistry of these star
s has important similarities and differences, The near-solar abundance
s of the alpha-capture elements places these stars on the metal-rich e
xtension of McWilliam & Rich [1994, ApJS, 91, 749], but their s-proces
s abundances are much lower than those of the bulge giants, These low
s-process values have been interpreted as the hallmark of an ancient s
tellar population, We are unable to convincingly assign these stars to
a known Galactic population and Lye urge further studies of larger sa
mples. (C) 1997 American Astronomical Society.