Abstract
Differences in the chemical composition of galactic stars with similar [Fe/H], in particular in the range −1.0 to +0.50 dex, are attributed to the presence of different stellar components in the Galaxy, in general, and in the Galactic disk, in particular (e.g. Norris, 1999). Detailed high resolution (HR) analysis is the most appropriate approach to determine individual element abundances of individual stars. This kind of approach, when not feasible, may be substituted by the study of selected low resolution absorption features. In Franchini et al. (2004a) we introduced four combinations of Lick/IDS indices, namely NaD vs Ca4227, NaD vs Mg2, NaD vs Mgb, and NaD vs CaMg, to identify Solar Scaled Abundance (SSA) and α-enhanced (Non Solar Scaled Abundance, NSSA) stars without previous knowledge of atmospheric parameter values. Our method was applied in Franchini et al. (2004b) to 402 stars with accurate estimates of [Fe/H]. In this paper we extend the analysis to a larger number of stars to better investigate the metallicity and kinematical properties of NSSA and SSA stars.
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Morossi, C., Franchini, M., di Marcantonio, P., Malagnini, M., Chavez, M., Rodriguez-Merino, L. (2006). Chemo-Dynamical Properties of F-G-K Stars in the −1.0<[Fe/H]< +0.50 Range. In: Randich, S., Pasquini, L. (eds) Chemical Abundances and Mixing in Stars in the Milky Way and its Satellites. ESO ASTROPHYSICS SYMPOSIA. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-34136-9_25
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DOI: https://doi.org/10.1007/978-3-540-34136-9_25
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