A UNIFORM ASTEROSEISMIC ANALYSIS OF 22 SOLAR-TYPE STARS OBSERVED BY KEPLER

被引：158

作者：

Mathur, S. ^{[1
]}

Metcalfe, T. S. ^{[1
,2
]}

Woitaszek, M. ^{[2
]}

Bruntt, H. ^{[3
,4
]}

Verner, G. A. ^{[5
]}

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

Creevey, O. L. ^{[6
]}

Dogan, G. ^{[1
,3
]}

Basu, S. ^{[7
]}

Karoff, C. ^{[3
,5
]}

Stello, D. ^{[8
]}

Appourchaux, T. ^{[9
]}

Campante, T. L. ^{[3
,10
,11
]}

Chaplin, W. J. ^{[5
]}

Garcia, R. A. ^{[12
,13
]}

Bedding, T. R. ^{[8
]}

Benomar, O. ^{[8
]}

Bonanno, A. ^{[14
]}

Deheuvels, S. ^{[7
]}

Elsworth, Y. ^{[5
]}

Gaulme, P. ^{[9
]}

Guzik, J. A. ^{[15
]}

Handberg, R. ^{[3
]}

Hekker, S. ^{[5
,16
]}

Herzberg, W. ^{[17
]}

Monteiro, M. J. P. F. G. ^{[10
,11
]}

Piau, L. ^{[18
]}

Quirion, P. -O. ^{[19
]}

Regulo, C. ^{[20
,21
]}

Roth, M. ^{[16
]}

Salabert, D. ^{[6
]}

Serenelli, A. ^{[22
]}

Thompson, M. J. ^{[1
]}

Trampedach, R. ^{[23
,24
]}

White, T. R. ^{[8
]}

Ballot, J. ^{[25
,26
]}

Brandao, I. M. ^{[10
,11
]}

Molenda-Zakowicz, J. ^{[27
]}

Kjeldsen, H. ^{[3
]}

Twicken, J. D. ^{[28
]}

Uddin, K. ^{[29
]}

Wohler, B. ^{[29
]}

机构：

[1] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA

[2] Natl Ctr Atmospher Res, Computat & Informat Syst Lab, Boulder, CO 80307 USA

[3] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark

[4] Univ Paris 07, Univ Paris 06, UMR8109, LESIA,Obs Paris, F-92195 Meudon, France

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

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

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

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

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

[10] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal

[11] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal

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

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

[14] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy

[15] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

[16] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands

[17] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany

[18] LATMOS, F-78280 Guyancourt, France

[19] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada

[20] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain

[21] Inst Astrofis Canarias, Tenerife 38205, Spain

[22] Inst Ciencias Espacio CSIC IEEC, Fac Ciencias, Bellaterra 08193, Spain

[23] Univ Colorado, JILA, Boulder, CO 80309 USA

[24] Natl Inst Stand & Technol, Boulder, CO 80309 USA

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

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

[27] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland

[28] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA

[29] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 749卷 / 02期

基金：

美国国家科学基金会;

关键词：

methods: numerical; stars: evolution; stars: interiors; stars: oscillations; STELLAR EVOLUTION CODE; MODE FREQUENCY-SHIFTS; EQUATION-OF-STATE; SUN-LIKE STAR; BOLOMETRIC CORRECTIONS; MIXING-LENGTH; NGC; 6819; OSCILLATIONS; PARAMETERS; DIAGRAMS;

D O I：

10.1088/0004-637X/749/2/152

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Asteroseismology with the Kepler space telescope is providing not only an improved characterization of exoplanets and their host stars, but also a new window on stellar structure and evolution for the large sample of solar-type stars in the field. We perform a uniform analysis of 22 of the brightest asteroseismic targets with the highest signal-to-noise ratio observed for 1 month each during the first year of the mission, and we quantify the precision and relative accuracy of asteroseismic determinations of the stellar radius, mass, and age that are possible using various methods. We present the properties of each star in the sample derived from an automated analysis of the individual oscillation frequencies and other observational constraints using the Asteroseismic Modeling Portal (AMP), and we compare them to the results of model-grid-based methods that fit the global oscillation properties. We find that fitting the individual frequencies typically yields asteroseismic radii and masses to similar to 1% precision, and ages to similar to 2.5% precision (respectively, 2, 5, and 8 times better than fitting the global oscillation properties). The absolute level of agreement between the results from different approaches is also encouraging, with model-grid-based methods yielding slightly smaller estimates of the radius and mass and slightly older values for the stellar age relative to AMP, which computes a large number of dedicated models for each star. The sample of targets for which this type of analysis is possible will grow as longer data sets are obtained during the remainder of the mission.

引用

页数：14

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