STELLAR AGES AND CONVECTIVE CORES IN FIELD MAIN-SEQUENCE STARS: FIRST ASTEROSEISMIC APPLICATION TO TWO KEPLER TARGETS

被引：95

作者：

Aguirre, V. Silva ^{[1
,2
,3
]}

Basu, S. ^{[4
]}

Brandao, I. M. ^{[5
,6
]}

Christensen-Dalsgaard, J. ^{[1
,3
]}

Deheuvels, S. ^{[4
,7
,8
]}

Dogan, G. ^{[9
]}

Metcalfe, T. S. ^{[10
]}

Serenelli, A. M. ^{[3
,11
]}

Ballot, J. ^{[7
,8
]}

Chaplin, W. J. ^{[1
,3
,12
]}

Cunha, M. S. ^{[5
,6
]}

Weiss, A. ^{[2
]}

Appourchaux, T. ^{[13
]}

Casagrande, L. ^{[14
]}

Cassisi, S. ^{[15
]}

Creevey, O. L. ^{[16
]}

Garcia, R. A. ^{[3
,17
,18
]}

Lebreton, Y. ^{[19
,20
]}

Noels, A. ^{[21
]}

Sousa, S. G. ^{[5
,6
]}

Stello, D. ^{[22
]}

White, T. R. ^{[22
]}

Kawaler, S. D. ^{[23
]}

Kjeldsen, H. ^{[1
]}

机构：

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

[2] Max Planck Inst Astrophys, D-85748 Garching, Germany

[3] Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA

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

[5] Univ Porto, Ctr Astrofis, P-4150762 Porto, Portugal

[6] Univ Porto, Fac Ciencias, P-4150762 Porto, Portugal

[7] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France

[8] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France

[9] NCAR, High Altitude Observ, Boulder, CO 80307 USA

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

[11] Fac Ciencies, IEEC, CSIC, Inst Ciencias Espacio, E-08193 Barcelona, Spain

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

[13] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France

[14] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia

[15] Astron Observ Teramo, INAF, I-64100 Teramo, Italy

[16] Univ Nice Sophia Antipolis, Lab Lagrange, F-06300 Nice, France

[17] Univ Paris Diderot, CNRS, CEA, Lab AIM,DSM, F-91191 Gif Sur Yvette, France

[18] Ctr Saclay, IRFU SAp, F-91191 Gif Sur Yvette, France

[19] Observ Paris, CNRS, GEPI, UMR 8111, F-92195 Meudon, France

[20] Univ Rennes 1, CNRS, UMR 6251, Inst Phys Rennes, F-35042 Rennes, France

[21] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium

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

[23] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 769卷 / 02期

基金：

美国国家科学基金会; 英国科学技术设施理事会; 欧洲研究理事会; 新加坡国家研究基金会;

关键词：

asteroseismology; stars: fundamental parameters; stars: interiors; stars: oscillations; SOLAR-TYPE STARS; COLOR-MAGNITUDE DIAGRAM; EQUATION-OF-STATE; DELTA-Y/DELTA-Z; OSCILLATION FREQUENCIES; AUTOMATIC-DETERMINATION; ACOUSTIC-OSCILLATIONS; CHEMICAL-COMPOSITION; GLOBULAR-CLUSTERS; PHASE-SHIFT;

D O I：

10.1088/0004-637X/769/2/141

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using asteroseismic data and stellar evolution models we obtain the first detection of a convective core in a Kepler field main-sequence star, putting a stringent constraint on the total size of the mixed zone and showing that extra mixing beyond the formal convective boundary exists. In a slightly less massive target the presence of a convective core cannot be conclusively discarded, and thus its remaining main-sequence lifetime is uncertain. Our results reveal that best-fit models found solely by matching individual frequencies of oscillations corrected for surface effects do not always properly reproduce frequency combinations. Moreover, slightly different criteria to define what the best-fit model is can lead to solutions with similar global properties but very different interior structures. We argue that the use of frequency ratios is a more reliable way to obtain accurate stellar parameters, and show that our analysis in field main-sequence stars can yield an overall precision of 1.5%, 4%, and 10% in radius, mass, and age, respectively. We compare our results with those obtained from global oscillation properties, and discuss the possible sources of uncertainties in asteroseismic stellar modeling where further studies are still needed.

引用

页数：17

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