The Gaia-ESO Survey: the origin and evolution of s-process elements

被引：51

作者：

Magrini, L. ^{[1
]}

Spina, L. ^{[2
]}

Randich, S. ^{[1
]}

Friel, E. ^{[3
]}

Kordopatis, G. ^{[4
]}

Worley, C. ^{[5
]}

Pancino, E. ^{[1
,6
]}

Bragaglia, A. ^{[7
]}

Donati, P. ^{[7
]}

Tautvaisiene, G. ^{[8
]}

Bagdonas, V. ^{[8
]}

Delgado-Mena, E. ^{[9
]}

Adibekyan, V. ^{[9
]}

Sousa, S. G. ^{[9
]}

Jimenez-Esteban, F. M. ^{[10
]}

Sanna, N. ^{[1
]}

Roccatagliata, V. ^{[1
]}

Bonito, R. ^{[11
]}

Sbordone, L. ^{[12
]}

Duffau, S. ^{[13
]}

Gilmore, G. ^{[5
]}

Feltzing, S. ^{[14
]}

Jeffries, R. D. ^{[15
]}

Vallenari, A. ^{[16
]}

Alfaro, E. J. ^{[17
]}

Bensby, T. ^{[14
]}

Francois, P. ^{[18
]}

Koposov, S. ^{[5
]}

Korn, A. J. ^{[19
]}

Recio-Blanco, A. ^{[20
]}

Smiljanic, R. ^{[21
]}

Bayo, A. ^{[22
,23
]}

Carraro, G. ^{[24
]}

Casey, A. R. ^{[2
]}

Costado, M. T. ^{[25
]}

Damiani, F. ^{[11
]}

Franciosini, E. ^{[1
]}

Frasca, A. ^{[26
]}

Hourihane, A. ^{[5
]}

Jofre, P. ^{[27
]}

de Laverny, P. ^{[20
]}

Lewis, J. ^{[5
]}

Masseron, T. ^{[28
,29
]}

Monaco, L. ^{[13
]}

Morbidelli, L. ^{[1
]}

Prisinzano, L. ^{[11
]}

Sacco, G. ^{[1
]}

Zaggia, S. ^{[16
]}

机构：

[1] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy

[2] Monash Univ, Sch Phys & Astron, Monash Ctr Astrophys, Clayton, Vic 3800, Australia

[3] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA

[4] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, Nice, France

[5] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[6] Agenzia Spaziale Italiana, Space Sci Data Ctr, Via Politecn SNC, I-00133 Rome, Italy

[7] Osservatorio Astrofis & Sci Spazio, INAF, Via Gobetti 93-3, I-40129 Bologna, Italy

[8] Vilnius Univ, Inst Theoret Phys & Astron, Astron Observ, Ave Sauletekio Al 3, LT-10257 Vilnius, Lithuania

[9] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, P-4150762 Porto, Portugal

[10] CSIC, INTA, Ctr Astrobiol, Dept Astrofis, ESAC Campus,Camino Bajo del Castillo S-N, Madrid 28692, Spain

[11] Osserv Astron Palermo, INAF, Piazza Parlamento 1, I-90134 Palermo, Italy

[12] European Southern Observ, Alonso de Cordova 3107 Vitacura, Santiago, Chile

[13] Univ Andres Bello, Dept Ciencias Fis, Fernandez Concha 700, Santiago, Chile

[14] Lund Observ, Dept Astron & Theoret Phys, Box 43, S-22100 Lund, Sweden

[15] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England

[16] Padova Observ, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy

[17] CSIC, Inst Astrofis Andalucia, Apdo 3004, E-18080 Granada, Spain

[18] Univ Paris Diderot, CNRS, Observ Paris, GEPI, 5 Pl Jules Janssen, F-92190 Meudon, France

[19] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden

[20] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, Lab Lagrange,UMR7293, CS 34229, F-06304 Nice 4, France

[21] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland

[22] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile

[23] Univ Valparaiso, Millennium Nucleus Nucleo Planet Format, Valparaiso, Chile

[24] Univ Padua, Dipartimento Fis & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy

[25] Univ Cadiz, Dept Didact, Cadiz 11519, Spain

[26] Osserv Astrofis Catania, INAF, Via S Sofia 78, I-95123 Catania, Italy

[27] Univ Diego Portales, Fac Ingn, Nucleo Astron, Ave Ejercito 441, Santiago, Chile

[28] Inst Astrofis Canarias, Tenerife 38205, Spain

[29] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 617卷

基金：

欧盟地平线“2020”; 英国科学技术设施理事会;

关键词：

Galaxy: abundances; open clusters and associations: general; Galaxy: disk; GALACTIC CHEMICAL EVOLUTION; GIANT BRANCH STARS; OPEN CLUSTERS; NEUTRON-CAPTURE; AGB STARS; NUCLEOSYNTHESIS; BARIUM; ABUNDANCES; PHOTOMETRY; DEPENDENCE;

D O I：

10.1051/0004-6361/201832841

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Several works have found an increase of the abundances of the s-process neutron-capture elements in the youngest Galactic stellar populations. These trends provide important constraints on stellar and Galactic evolution and they need to be confirmed with large and statistically significant samples of stars spanning wide age and distance intervals. Aims. We aim to trace the abundance patterns and the time evolution of five s-process elements - two belonging to the first peak, Y and Zr, and three belonging to the second peak, Ba, La, and Ce - using the Gaia-ESO DRS results for open clusters and disc stars. Methods. From the UVES spectra of cluster member stars, we determined the average composition of clusters with ages >0.1 Gyr. We derived statistical ages and distances of field stars, and we separated them into thin and thick disc populations. We studied the time-evolution and dependence on metallicity of abundance ratios using open clusters and field stars whose parameters and abundances were derived in a homogeneous way. Results. Using our large and homogeneous sample of open clusters, thin and thick disc stars, spanning an age range larger than 10 Gyr, we confirm an increase towards young ages of s-process abundances in the solar neighbourhood. These trends are well defined for open clusters and stars located nearby the solar position and they may be explained by a late enrichment due to significant contribution to the production of these elements from long-living low-mass stars. At the same time, we find a strong dependence of the s-process abundance ratios on the Galactocentric distance and on the metallicity of the clusters and field stars. Conclusions. Our results, derived from the largest and most homogeneous sample of s-process abundances in the literature, confirm the growth with decreasing stellar ages of the s-process abundances in both field and open cluster stars. At the same time, taking advantage of the abundances of open clusters located in a wide Galactocentric range, these results offer a new perspective on the dependence of the s-process evolution on the metallicity and star formation history, pointing to different behaviours at various Galactocentric distances.

引用

页数：15

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