Reference : The Gaia-ESO Survey: Sodium and aluminium abundances in giants and dwarfs. Implicatio...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/205399
The Gaia-ESO Survey: Sodium and aluminium abundances in giants and dwarfs. Implications for stellar and Galactic chemical evolution
English
Smiljanic, R. [Department for Astrophysics, Nicolaus Copernicus Astronomical Center, ul. Rabiańska 8, 87-100, Toruń, Poland]
Romano, D. [INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127, Bologna, Italy]
Bragaglia, A. [INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127, Bologna, Italy]
Donati, P. [INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127, Bologna, Italy; Dipartimento di Fisica e Astronomia, Università di Bologna, via Ranzani 1, 40127, Bologna, Italy]
Magrini, L. [INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5 , 50125, Firenze, Italy]
Friel, E. [Department of Astronomy, Indiana University, Bloomington, IN, 47405, USA]
Jacobson, H. [Kavli Institute for Astrophysics & Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA, 02139, USA]
Randich, S. [INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5 , 50125, Firenze, Italy]
Ventura, P. [INAF-Osservatorio Astronomico di Roma, via Frascati 33, 00040, Monte Porzio Catone, RM, Italy]
Lind, K. [Department of Physics and Astronomy, Uppsala University, Box 516, 751 20, Uppsala, Sweden; Max Planck Institute für Astronomy, Königstuhl 17, 69117, Heidelberg, Germany]
Bergemann, M. [Max Planck Institute für Astronomy, Königstuhl 17, 69117, Heidelberg, Germany]
Nordlander, T. [Department of Physics and Astronomy, Uppsala University, Box 516, 751 20, Uppsala, Sweden]
Morel, Thierry mailto [Université de Liège > > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Pancino, E. [INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127, Bologna, Italy; ASI Science Data Center, via del Politecnico SNC, 00133, Roma, Italy]
Tautvaišienė, G. [Institute of Theoretical Physics and Astronomy, Vilnius University, Goštauto 12, 01108, Vilnius, Lithuania]
Adibekyan, V. [Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762, Porto, Portugal]
Tosi, M. [INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127, Bologna, Italy]
Vallenari, A. [INAF-Osservatorio Astronomico di Padova, Vicolo Osservatorio 2, 35122, Padova, Italy]
Gilmore, G. [Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK]
Bensby, T. [Lund Observatory, Department of Astronomy and Theoretical Physics, Box 43, 221 00, Lund, Sweden]
François, Pauline [> > > >]
Koposov, S. [Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK]
Lanzafame, A. C. [Dipartimento di Fisica e Astronomia, Sezione Astrofisica, Universitá di Catania, via S. Sofia 78, 95123, Catania, Italy]
Recio-Blanco, A. [Laboratoire Lagrange (UMR7293), Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, CS 34229, 06304, Nice Cedex 4, France]
Bayo, A. [Instituto de Física y Astronomía, Universidad de Valparaíso, Chile]
Carraro, G. [European Southern Observatory, Alonso de Cordova 3107 Vitacura, Santiago de Chile, Chile]
Casey, A. R. [Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK]
Costado, M. T. [Instituto de Astrofísica de Andalucía-CSIC, Apdo. 3004, 18080, Granada, Spain]
Franciosini, E. [INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5 , 50125, Firenze, Italy]
Heiter, U. [Department of Physics and Astronomy, UppsalaUniversity, Box 516, 751 20, Uppsala, Sweden]
Hill, V. [Laboratoire Lagrange (UMR7293), Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, CS 34229, 06304, Nice Cedex 4, France]
Hourihane, A. [Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK]
Jofré, P. [Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK]
Lardo, C. [Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool, L3 5RF, UK]
de Laverny, P. [Laboratoire Lagrange (UMR7293), Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, CS 34229, 06304, Nice Cedex 4, France]
Lewis, J. [Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK]
Monaco, L. [Departamento de Ciencias Fisicas, Universidad Andres Bello, Republica 220, Santiago, Chile]
Morbidelli, L. [INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5 , 50125, Firenze, Italy]
Sacco, G. G. [INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5 , 50125, Firenze, Italy]
Sbordone, L. [Millennium Institute of Astrophysics, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile; Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile]
Sousa, S. G. [Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762, Porto, Portugal]
Worley, C. C. [Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK]
Zaggia, S. [INAF-Osservatorio Astronomico di Padova, Vicolo Osservatorio 2, 35122, Padova, Italy)]
1-May-2016
Astronomy and Astrophysics
EDP Sciences
589
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] Galaxy: abundances ; Galaxy: evolution ; stars: abundances ; stars: evolution ; stars: late-type
[en] Context. Stellar evolution models predict that internal mixing should cause some sodium overabundance at the surface of red giants more massive than ~1.5-2.0 M[SUB]⊙[/SUB]. 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. <BR /> Aims: 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. <BR /> Methods: 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. <BR /> Results: Abundances of Na in stars with mass below ~2.0 M[SUB]⊙[/SUB], and of Al in stars below ~3.0 M[SUB]⊙[/SUB], 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[SUB]⊙[/SUB], 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. Based on observations made with the ESO/VLT, at Paranal Observatory, under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey), and on data obtained from the ESO Archive originally observed under programs 60.A-9143, 076.B-0263 and 082.D-0726.Table 1 is only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/589/A115">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/589/A115</A>
http://hdl.handle.net/2268/205399
10.1051/0004-6361/201528014
http://adsabs.harvard.edu/abs/2016A%26A...589A.115S

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