Volume 367, Number 1, February III 2001
|Page(s)||253 - 265|
|Section||Interstellar and circumstellar matter|
|Published online||15 February 2001|
The nature of super-metal-rich stars*
Detailed abundance analysis of 8 super-metal-rich star candidates
Lund Observatory, Box 43, 221 00 Lund, Sweden
2 Astronomy Department, University of Washington, PO Box 351580, Seattle, WA 98195, USA
Corresponding author: S. Feltzing, firstname.lastname@example.org
Accepted: 17 November 2000
We provide detailed abundance analyses of 8 candidate super-metal-rich stars. Five of them are confirmed to have dex, the generally-accepted limit for super-metal-richness. Furthermore, we derive abundances of several elements and find that the stars follow trends seen in previous studies of metal-rich stars. Ages are estimated from isochrones and velocities calculated. We find that there do exist very metal-rich stars that are older than 10 Gyr. This is contrary to what is found in several recent studies of the galactic age-metallicity relation. This is tentative evidence that there might not exist a one-to-one relation between age and metallicity for all stars. This is not surprising considering the current models of the independent evolution of the different galactic components. We also find that one star, HD 182572, could with ∼75% chance be a thick disk star with, for the thick disk, an extremely high metallicity at 0.34 dex. This star is, intriguingly, also somewhat enhanced in the α-elements.
Key words: stars: abundances, fundamental parameters, late-type, individual HD 10780, HD 32147, HD 99491, HD 104304, HD 121370, HD 145675, HD 196755, HD 182572 / Galaxy: solar neighbourhood
© ESO, 2001
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