Young α-enriched giant stars in the solar neighbourhood

被引：145

作者：

Martig, Marie ^{[1
]}

Rix, Hans-Walter ^{[1
]}

Aguirre, Victor Silva ^{[2
]}

Hekker, Saskia ^{[2
,3
]}

Mosser, Benoit ^{[4
]}

Elsworth, Yvonne ^{[5
]}

Bovy, Jo ^{[6
]}

Stello, Dennis ^{[2
,7
]}

Anders, Friedrich ^{[8
]}

Garcia, Rafael A. ^{[9
]}

Tayar, Jamie ^{[10
]}

Rodrigues, Thaise S. ^{[11
,12
,13
]}

Basu, Sarbani ^{[14
]}

Carrera, Ricardo ^{[15
,16
]}

Ceillier, Tugdual ^{[9
]}

Chaplin, William J. ^{[2
,5
]}

Chiappini, Cristina ^{[8
]}

Frinchaboy, Peter M. ^{[17
]}

Garcia-Hernandez, D. A. ^{[15
,16
]}

Hearty, Fred R. ^{[18
]}

Holtzman, Jon ^{[19
]}

Johnson, Jennifer A. ^{[10
]}

Majewski, Steven R. ^{[20
]}

Mathur, Savita ^{[21
]}

Meszaros, Szabolcs ^{[22
]}

Miglio, Andrea ^{[2
,5
]}

Nidever, David ^{[23
]}

Pan, Kaike ^{[24
]}

Pinsonneault, Marc ^{[10
]}

Schiavon, Ricardo P. ^{[25
]}

Schneider, Donald P. ^{[18
,26
]}

Serenelli, Aldo ^{[27
]}

Shetrone, Matthew ^{[28
]}

Zamora, Olga ^{[15
,16
]}

机构：

[1] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[2] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark

[3] Max Planck Inst Sonnensystemforsch, D-37077 Gottingen, Germany

[4] Univ Paris 07, CNRS, LESIA, Univ Paris 06,Observ Paris, F-92195 Meudon, France

[5] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England

[6] Inst Adv Study, Princeton, NJ 08540 USA

[7] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW 2006, Australia

[8] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany

[9] Univ Paris Diderot IRFU SAp, Ctr Saclay, Lab AIM, CEA DSM,CNRS, F-91191 Gif Sur Yvette, France

[10] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA

[11] Osservatorio Astron Padova INAF, I-35122 Padua, Italy

[12] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy

[13] La Interinst eAstron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil

[14] Yale Univ, Dept Astron, New Haven, CT 06520 USA

[15] Inst Astrofis Canarias, E-38205 Tenerife, Spain

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

[17] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA

[18] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[19] New Mexico State Univ, Las Cruces, NM 88003 USA

[20] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA

[21] Space Sci Inst, Boulder, CO 80301 USA

[22] ELTE Gothard Astrophys Observ, H-9704 Szombathely, Hungary

[23] Univ Michigan, Dept Astron, Ann Arbor, MI 48104 USA

[24] Apache Point Observ, Sunspot, NM 88349 USA

[25] Liverpool John Moores Univ, Res Inst, Liverpool L3 5RF, Merseyside, England

[26] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA

[27] Inst Space Sci CSIC IEEC, E-08193 Bellaterra, Catalunya, Spain

[28] Univ Texas Austin, McDonald Observ, Austin, TX 79734 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2015年 / 451卷 / 02期

基金：

欧洲研究理事会; 美国国家科学基金会; 澳大利亚研究理事会; 英国科学技术设施理事会; 美国安德鲁·梅隆基金会; 新加坡国家研究基金会;

关键词：

stars: abundances; stars: fundamental parameters; STELLAR EVOLUTION DATABASE; METAL-POOR STARS; DELTA-Y/DELTA-Z; RED GIANTS; MILKY-WAY; CHEMICAL EVOLUTION; NGC; 6791; FUNDAMENTAL PROPERTIES; GALACTIC ARCHAEOLOGY; POPULATION SYNTHESIS;

D O I：

10.1093/mnras/stv1071

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We derive age constraints for 1639 red giants in the APOKASC sample for which seismic parameters from Kepler, as well as effective temperatures, metallicities and [alpha/Fe] values from APOGEE DR12 (Apache Point Observatory Galactic Evolution Experiment Data Release 12) are available. We investigate the relation between age and chemical abundances for these stars, using a simple and robust approach to obtain ages. We first derive stellar masses using standard seismic scaling relations, then determine the maximum possible age for each star as function of its mass and metallicity, independently of its evolutionary stage. While the overall trend between maximum age and chemical abundances is a declining fraction of young stars with increasing [alpha/Fe], at least 14 out of 241 stars with [alpha/Fe] >0.13 are younger than 6 Gyr. Five stars with [alpha/Fe] >= 0.2 have ages below 4 Gyr. We examine the effect of modifications in the standard seismic scaling relations, as well as the effect of very low helium fractions, but these changes are not enough to make these stars as old as usually expected for alpha-rich stars (i.e. ages greater than 8-9 Gyr). Such unusual alpha-rich young stars have also been detected by other surveys, but defy simple explanations in a galaxy evolution context.

引用

页码：2230 / 2243

页数：14

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