The Gaia-ESO Survey: Evidence of atomic diffusion in M67?

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dc.contributor.authorBertelli Motta C.
dc.contributor.authorPasquali A.
dc.contributor.authorRicher J.
dc.contributor.authorMichaud G.
dc.contributor.authorSalaris M.
dc.contributor.authorBragaglia A.
dc.contributor.authorMagrini L.
dc.contributor.authorRandich S.
dc.contributor.authorGrebel E.K.
dc.contributor.authorAdibekyan V.
dc.contributor.authorBlanco-Cuaresma S.
dc.contributor.authorDrazdauskas A.
dc.contributor.authorFu X.
dc.contributor.authorMartell S.
dc.contributor.authorTautvaišiene G.
dc.contributor.authorGilmore G.
dc.contributor.authorAlfaro E.J.
dc.contributor.authorBensby T.
dc.contributor.authorFlaccomio E.
dc.contributor.authorKoposov S.E.
dc.contributor.authorKorn A.J.
dc.contributor.authorLanzafame A.C.
dc.contributor.authorSmiljanic R.
dc.contributor.authorBayo A.
dc.contributor.authorCarraro G.
dc.contributor.authorCasey A.R.
dc.contributor.authorCostado M.T.
dc.contributor.authorDamiani F.
dc.contributor.authorFranciosini E.
dc.contributor.authorHeiter U.
dc.contributor.authorHourihane A.
dc.contributor.authorJofré P.
dc.contributor.authorLardo C.
dc.contributor.authorLewis J.
dc.contributor.authorMonaco L.
dc.contributor.authorMorbidelli L.
dc.contributor.authorSousa S.G.
dc.contributor.authorWorley C.C.
dc.contributor.authorZaggia S.
dc.contributor.authorSacco, G.G.
dc.date.accessioned2022-07-27T22:28:54Z
dc.date.available2022-07-27T22:28:54Z
dc.date.issued2018-07
dc.descriptionIndexación Scopuses
dc.description.abstractInvestigating the chemical homogeneity of stars born from the same molecular cloud at virtually the same time is very important for our understanding of the chemical enrichment of the interstellar medium and with it the chemical evolution of the Galaxy. One major cause of inhomogeneities in the abundances of open clusters is stellar evolution of the cluster members. In this work, we investigate variations in the surface chemical composition of member stars of the old open clusterM67 as a possible consequence of atomic diffusion effects taking place during the main-sequence phase. The abundances used are obtained from high-resolution UVES/FLAMES spectra within the framework of the Gaia-ESO Survey. We find that the surface abundances of stars on the main sequence decrease with increasing mass reaching a minimum at the turn-off. After deepening of the convective envelope in subgiant branch stars, the initial surface abundances are restored.We found themeasured abundances to be consistent with the predictions of stellar evolutionary models for a cluster with the age and metallicity of M67. Our findings indicate that atomic diffusion poses a non-negligible constraint on the achievable precision of chemical tagging methods. © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.es
dc.description.urihttps://academic-oup-com.recursosbiblioteca.unab.cl/mnras/article/478/1/425/4983131
dc.identifier.citationMonthly Notices of the Royal Astronomical Society Volume 478, Issue 1, Pages 425 - 43821 July 2018es
dc.identifier.doi10.1093/mnras/sty1011
dc.identifier.issn00358711
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/23362
dc.language.isoenes
dc.publisherOxford University Presses
dc.rights.licenseCC BY 4.0
dc.subjectOpen Clusterses
dc.subjectMagellanic Cloudses
dc.subjectGaiaes
dc.subjectAtomic diffusionses
dc.subjectGalaxies abundanceses
dc.titleThe Gaia-ESO Survey: Evidence of atomic diffusion in M67?es
dc.typeArtículoes
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