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dc.contributor.authorChiappini, C.C.M.pt_BR
dc.contributor.authorAnders, Friedrichpt_BR
dc.contributor.authorRodrigues, Thaise da Silvapt_BR
dc.contributor.authorMiglio, Andreapt_BR
dc.contributor.authorMontalbán, Josefinapt_BR
dc.contributor.authorMosser, Benoîtpt_BR
dc.contributor.authorGirardi, Leo Albertopt_BR
dc.contributor.authorValentini, Maricapt_BR
dc.contributor.authorNoels, Arlettept_BR
dc.contributor.authorMorel , Thierrypt_BR
dc.contributor.authorMinchev, Ivanpt_BR
dc.contributor.authorSteinmetz, M.pt_BR
dc.contributor.authorSantiago, Basilio Xavierpt_BR
dc.contributor.authorSchultheis, Mathiaspt_BR
dc.contributor.authorMartig, Mariept_BR
dc.contributor.authorCosta, Luiz N. dapt_BR
dc.contributor.authorMaia, Marcio Antonio Geimbapt_BR
dc.contributor.authorAllende Prieto, Carlospt_BR
dc.contributor.authorAssis Peralta, R. dept_BR
dc.contributor.authorHekker, Saskiapt_BR
dc.contributor.authorThemeßl, Nathaliept_BR
dc.contributor.authorKallinger, Thomaspt_BR
dc.contributor.authorGarcia, Rafael A.pt_BR
dc.contributor.authorMathur, Savitapt_BR
dc.contributor.authorBaudin, Fredericpt_BR
dc.contributor.authorBeers, T.C.pt_BR
dc.contributor.authorCunha, Katiapt_BR
dc.contributor.authorHarding, Paulpt_BR
dc.contributor.authorHoltzman, J.A.pt_BR
dc.contributor.authorMajewski, Steven Raymondpt_BR
dc.contributor.authorMészáros, S.pt_BR
dc.contributor.authorNidever, D.L.pt_BR
dc.contributor.authorPan, K.pt_BR
dc.contributor.authorSchiavon, Ricardo P.pt_BR
dc.contributor.authorShetrone, M.pt_BR
dc.contributor.authorSchneider, D.P.pt_BR
dc.contributor.authorStassun, Keivan G.pt_BR
dc.date.accessioned2016-07-22T02:17:27Zpt_BR
dc.date.issued2015pt_BR
dc.identifier.issn0004-6361pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/143886pt_BR
dc.description.abstractWe report the discovery of a group of apparently young CoRoT red-giant stars exhibiting enhanced [ /Fe] abundance ratios (as determined from APOGEE spectra) with respect to solar values. Their existence is not explained by standard chemical evolution models of the Milky Way, and shows that the chemical-enrichment history of the Galactic disc is more complex. We find similar stars in previously published samples for which isochrone-ages could be reliably obtained, although in smaller relative numbers. This might explain why these stars have not previously received attention. The young [ /Fe]-rich stars are much more numerous in the CoRoT-APOGEE (CoRoGEE) inner-field sample than in any other high-resolution sample available at present because only CoRoGEE can explore the inner-disc regions and provide ages for its field stars. The kinematic properties of the young [ /Fe]-rich stars are not clearly thick-disc like, despite their rather large distances from the Galactic mid-plane. Our tentative interpretation of these and previous intriguing observations in the Milky Way is that these stars were formed close to the end of the Galactic bar, near corotation – a region where gas can be kept inert for longer times than in other regions that are more frequently shocked by the passage of spiral arms. Moreover, this is where the mass return from older inner-disc stellar generations is expected to be highest (according to an inside-out disc-formation scenario), which additionally dilutes the in-situ gas. Other possibilities to explain these observations (e.g., a recent gas-accretion event) are also discussed.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofAstronomy and astrophysics. Les Ulis. Vol. 576 (Apr. 2015), L12, 7 p.pt_BR
dc.rightsOpen Accessen
dc.subjectGalaxy: abundancesen
dc.subjectFormacao de galaxiaspt_BR
dc.subjectGalaxy: formationen
dc.subjectAsterosismologiapt_BR
dc.subjectGalaxy: disken
dc.subjectGalaxy: stellar contenten
dc.subjectStars: fundamental parametersen
dc.subjectAsteroseismologyen
dc.titleYoung (α/Fe)-enhanced stars discovered by CoRoT and APOGEE : what is their origin?pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000996899pt_BR
dc.type.originEstrangeiropt_BR


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