Astrophysics
[Submitted on 15 Apr 2003 (v1), last revised 30 Apr 2003 (this version, v2)]
Title:Detailed Analysis of Nearby Bulgelike Dwarf Stars III. Alpha and Heavy-element abundances
View PDFAbstract: The present sample of nearby bulgelike dwarf stars has kinematics and metallicities characteristic of a probable inner disk or bulge origin. Ages derived by using isochrones give 10-11 Gyr for these stars and metallicities are in the range -0.80< [Fe/H]< +0.40. We calculate stellar parameters from spectroscopic data, and chemical abundances of Mg, Si, Ca, Ti, La, Ba, Y, Zr and Eu are derived by using spectrum synthesis.
We found that [alpha-elements/Fe] show different patterns depending on the element. Si, Ca and Ti-to-iron ratios decline smoothly for increasing metallicities, and follow essentially the disk pattern. O and Mg, products of massive supernovae, and also the r-process element Eu, are overabundant relative to disk stars, showing a steeper decline for metallicities [Fe/H] > -0.3 dex. [s-elements/Fe] roughly track the solar values with no apparent trend with metallicity for [Fe/H] < 0, showing subsolar values for the metal rich stars. Both kinematical and chemical properties of the bulgelike stars indicate a distinct identity of this population when compared to disk stars.
Submission history
From: Luciana Pompeia [view email][v1] Tue, 15 Apr 2003 14:09:52 UTC (173 KB)
[v2] Wed, 30 Apr 2003 22:11:00 UTC (173 KB)
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