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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Analysis of old very metal rich stars in the solar neighbourhood

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Author(s):
Trevisan, M. [1] ; Barbuy, B. [1] ; Eriksson, K. [2] ; Gustafsson, B. [2] ; Grenon, M. [3] ; Pompeia, L. [4]
Total Authors: 6
Affiliation:
[1] Univ Sao Paulo, BR-05508900 Sao Paulo - Brazil
[2] Uppsala Univ, Dept Astron & Space Phys, S-75120 Uppsala - Sweden
[3] Observ Geneva, CH-1290 Sauverny - Switzerland
[4] Univ Vale Paraiba, BR-12244000 Sao Paulo - Brazil
Total Affiliations: 4
Document type: Journal article
Source: Astronomy & Astrophysics; v. 535, NOV 2011.
Web of Science Citations: 31
Abstract

Context. A sample of mostly old metal-rich dwarf and turn-off stars with high eccentricity and low maximum height above the Galactic plane has been identified. From their kinematics, it was suggested that the inner disk is their most probable birthplace. Their chemical imprints may therefore reveal important information about the formation and evolution of the still poorly understood inner disk. Aims. To probe the formation history of these stellar populations, a detailed analysis of a sample of very metal-rich stars is carried out. We derive the metallicities, abundances of a elements, ages, and Galactic orbits. Methods. The analysis of 71 metal-rich stars is based on optical high-resolution echelle spectra obtained with the FEROS spectrograph at the ESO 1.52-m Telescope at La Silla, Chile. The metallicities and abundances of C, O, Mg, Si, Ca, and Ti were derived based on LTE detailed analysis, employing the MARCS model atmospheres. Results. We confirm the high metallicity of these stars reaching up to {[}Fe-I/H] = 0.58, and the sample of metal-rich dwarfs can be kinematically subclassified in samples of thick disk, thin disk, and intermediate stellar populations. All sample stars show solar alpha-Fe ratios, and most of them are old and still quite metal rich. The orbits suggest that the thin disk, thick disk and intermediate populations were formed at Galactocentric distances of similar to 8 kpc, similar to 6 kpc, and similar to 7 kpc, respectively. The mean maximum height of the thick disk subsample of Z(max) similar to 380 pc, is lower than for typical thick disk stars. A comparison of a-element abundances of the sample stars with bulge stars shows that the oxygen is compatible with a bulge or inner thick disk origin. Our results suggest that models of radial mixing and dynamical effects of the bar and bar/spiral arms might explain the presence of these old metal-rich dwarf stars in the solar neighbourhood. (AU)