@Article{TrevisanBarb:2014:HeElOl,
               author = "Trevisan, Marina and Barbuy, B.",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         Universidade de S{\~a}o Paulo, Rua do Mat{\~a}o 1226S{\~a}o 
                         Paulo, Brazil",
                title = "Heavy elements in old very metal-rich stars",
              journal = "Astronomy \& Astrophysics",
                 year = "2014",
               volume = "570",
               number = "A22",
                pages = "13pp",
                month = "Oct.",
             keywords = "Heavy elements, Metal-rich stars, Solar neighborhood, Stars: 
                         abundances, Stars: atmosphere.",
             abstract = "Context. We studied a sample of high proper motion, old and 
                         metal-rich dwarf stars, selected from the NLTT catalogue. The low 
                         pericentric distances and eccentric orbits of these solar 
                         neighbourhood stars indicate that they might have originated in 
                         the inner parts of the Galaxy. Methods. The spectroscopic analysis 
                         is based on optical high-resolution {\'e}chelle spectra obtained 
                         with the FEROS spectrograph at the ESO 1.52 m Telescope at La 
                         Silla, Chile. The abundances of Y, Ba, La, and Eu were derived 
                         through LTE analysis, employing the MARCS model atmospheres. 
                         Results. The abundances of Y, Ba, La, and Eu vs. Fe and Mg as the 
                         reference elements indicate similarities between our sample of old 
                         metal-rich dwarf stars and the thin disk. On the other hand, the 
                         abundance ratios using O as the reference element, as well as 
                         their kinematics, suggest that our sample is clearly distinct from 
                         the thin-disk stars. They could be old inner thin-disk stars, as 
                         suggested previously, or bulge stars. In either cases, they would 
                         have migrated from the inner parts of the Galaxy to the solar 
                         neighbourhood. Aims. Chemical tagging can probe the formation 
                         history of stellar populations. To identify the origin of a sample 
                         of 71 very metal-rich dwarf stars, we derive the abundances of the 
                         neutron-capture elements Y, Ba, La, and Eu.",
                  doi = "10.1051/0004-6361/201322967",
                  url = "http://dx.doi.org/10.1051/0004-6361/201322967",
                 issn = "0004-6361 and 1432-0746",
                label = "scopus 2014-11 TrevisanBarb:2014:HeElOl",
             language = "en",
           targetfile = "1409.3543.pdf",
        urlaccessdate = "27 abr. 2024"
}