The Gaia-ESO Survey: Sodium and aluminium abundances in giants and dwarfs Implications for stellar and Galactic chemical evolution

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dc.contributor.authorSmiljanic, R.
dc.contributor.authorRomano, D.
dc.contributor.authorBragaglia, A.
dc.contributor.authorDonati, P.
dc.contributor.authorMagrini, L.
dc.contributor.authorFriel, E.
dc.contributor.authorJacobson, H.
dc.contributor.authorRandich, S.
dc.contributor.authorVentura, P.
dc.contributor.authorLind, K.
dc.contributor.authorBergemann, M.
dc.contributor.authorNordlander, T.
dc.contributor.authorMorel, T.
dc.contributor.authorPancino, E.
dc.contributor.authorTautvaisiene, G.
dc.contributor.authorAdibekyan, V.
dc.contributor.authorTosi, M.
dc.contributor.authorVallenari, A.
dc.contributor.authorGilmore, G.
dc.contributor.authorBensby, T.
dc.contributor.authorFrancois, P.
dc.contributor.authorKoposov, S.
dc.contributor.authorLanzafame, A. C.
dc.contributor.authorRecio Blanco, A.
dc.contributor.authorBayo, A.
dc.contributor.authorCarraro, G.
dc.contributor.authorCasey, A. R.
dc.contributor.authorCostado, M. T.
dc.contributor.authorFranciosini, E.
dc.contributor.authorHeiter, U.
dc.contributor.authorHill, V.
dc.contributor.authorHourihane, A.
dc.contributor.authorJofre, P.
dc.contributor.authorLardo, C.
dc.contributor.authorde Laverny, P.
dc.contributor.authorLewis, J.
dc.contributor.authorMonaco, L.
dc.contributor.authorMorbidelli, L.
dc.contributor.authorSacco, G. G.
dc.contributor.authorSbordone, L.
dc.contributor.authorSousa, S. G.
dc.contributor.authorWorley, C. C.
dc.contributor.authorZaggia, S.
dc.date.accessioned2024-01-10T12:09:35Z
dc.date.available2024-01-10T12:09:35Z
dc.date.issued2016
dc.description.abstractContext. Stellar evolution models predict that internal mixing should cause some sodium overabundance at the surface of red giants more massive than similar to 1.5-2.0 M-circle dot. The surface aluminium abundance should not be affected. Nevertheless, observational results disagree about the presence and/or the degree of Na and Al overabundances. In addition, Galactic chemical evolution models adopting different stellar yields lead to very different predictions for the behavior of [Na/Fe] and [Al/Fe] versus [Fe/H]. Overall, the observed trends of these abundances with metallicity are not well reproduced.
dc.description.abstractAims. We readdress both issues, using new Na and Al abundances determined within the Gaia-ESO Survey. Our aim is to obtain better observational constraints on the behavior of these elements using two samples: i) more than 600 dwarfs of the solar neighborhood and of open clusters and ii) low-and intermediate-mass clump giants in six open clusters.
dc.description.abstractMethods. Abundances were determined using high-resolution UVES spectra. The individual Na abundances were corrected for nonlocal thermodynamic equilibrium effects. For the Al abundances, the order of magnitude of the corrections was estimated for a few representative cases. For giants, the abundance trends with stellar mass are compared to stellar evolution models. For dwarfs, the abundance trends with metallicity and age are compared to detailed chemical evolution models.
dc.description.abstractResults. Abundances of Na in stars with mass below similar to 2.0 M-circle dot, and of Al in stars below similar to 3.0 M-circle dot, seem to be unaffected by internal mixing processes. For more massive stars, the Na overabundance increases with stellar mass. This trend agrees well with predictions of stellar evolutionary models. For Al, our only cluster with giants more massive than 3.0 M-circle dot, NGC 6705, is Al enriched. However, this might be related to the environment where the cluster was formed. Chemical evolution models that well fit the observed [Na/Fe] vs. [Fe/H] trend in solar neighborhood dwarfs cannot simultaneously explain the run of [Al/Fe] with [Fe/H], and vice versa. The comparison with stellar ages is hampered by severe uncertainties. Indeed, reliable age estimates are available for only a half of the stars of the sample. We conclude that Al is underproduced by the models, except for stellar ages younger than about 7 Gyr. In addition, some significant source of late Na production seems to be missing in the models. Either current Na and Al yields are affected by large uncertainties, and/or some important Galactic source(s) of these elements has as yet not been taken into account.
dc.description.funderNational Science Center of Poland
dc.description.funderBelspo
dc.description.funderFundacao para a Ciencia e a Tecnologia (FCT)
dc.description.funderResearch Council of Lithuania
dc.description.funderCNES
dc.description.funderSwedish National Space Board (SNSB)
dc.description.funderLa Silla Paranal Observatory
dc.description.funderUK Science and Technology Facilities Council
dc.description.funderEuropean Union FP7 programme through ERC
dc.description.funderLeverhulme Trust
dc.description.funderINAF
dc.description.funderMinistero dell' Istruzione, dell' Universita' e della Ricerca (MIUR)
dc.description.funderESF (European Science Foundation) through the GREAT Research Network Programme
dc.fechaingreso.objetodigital2024-05-07
dc.format.extent15 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/201528014
dc.identifier.issn1432-0746
dc.identifier.urihttps://doi.org/10.1051/0004-6361/201528014
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/76503
dc.identifier.wosidWOS:000375318300127
dc.information.autorucAstrofísica; Sbordone L;S/I;243032
dc.language.isoen
dc.nota.accesocontenido parcial
dc.publisherEDP SCIENCES S A
dc.revistaASTRONOMY & ASTROPHYSICS
dc.rightsacceso restringido
dc.subjectGalaxy: abundances
dc.subjectGalaxy: evolution
dc.subjectstars: abundances
dc.subjectstars: evolution
dc.subjectstars: late-type
dc.subjectRICH OPEN CLUSTER
dc.subjectMETAL-POOR STARS
dc.subjectPRE-MAIN-SEQUENCE
dc.subjectOLD OPEN CLUSTERS
dc.subjectRED GIANTS
dc.subjectELEMENTAL ABUNDANCES
dc.subjectEVOLVED STARS
dc.subjectLIGHT-METALS
dc.subjectTRUMPLER 20
dc.subjectHYDROSTATIC NUCLEOSYNTHESIS
dc.subject.ods11 Sustainable Cities and Communities
dc.subject.odspa11 Ciudades y comunidades sostenibles
dc.titleThe Gaia-ESO Survey: Sodium and aluminium abundances in giants and dwarfs Implications for stellar and Galactic chemical evolution
dc.typeartículo
dc.volumen589
sipa.codpersvinculados243032
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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