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CONSTRUCTING A ONE-SOLAR-MASS EVOLUTIONARY SEQUENCE USING ASTEROSEISMIC DATA FROM KEPLER

Identifieur interne : 004674 ( PascalFrancis/Curation ); précédent : 004673; suivant : 004675

CONSTRUCTING A ONE-SOLAR-MASS EVOLUTIONARY SEQUENCE USING ASTEROSEISMIC DATA FROM KEPLER

Auteurs : V. Silva Aguirre [Allemagne] ; W. J. Chaplin [Royaume-Uni] ; J. Ballot [France] ; S. Basu [États-Unis] ; T. R. Bedding [Australie] ; A. M. Serenelli [Espagne] ; G. A. Verner [Royaume-Uni] ; A. Miglio [Royaume-Uni] ; M. J. P. F. G. Monteiro [Portugal] ; A. Weiss [Allemagne] ; T. Appourchaux [France] ; A. Bonanno [Italie] ; A. M. Broomhall [Royaume-Uni] ; H. Bruntt [Danemark] ; T. L. Campante [Portugal, Danemark] ; L. Casagrande [Allemagne] ; E. Corsaro [Italie] ; Y. Elsworth [Royaume-Uni] ; R. A. Garcia [France] ; P. Gaulme [France] ; R. Handberg [Danemark] ; S. Hekker [Royaume-Uni, Pays-Bas] ; D. Huber [Australie] ; C. Karoff [Danemark] ; S. Mathur [États-Unis] ; B. Mosser [France] ; D. Salabert [France] ; R. Schönrich [Allemagne] ; S. G. Sousa [Portugal] ; D. Stello [Australie] ; T. R. White [Australie] ; J. Christensen-Dalsgaard [Danemark] ; R. L. Gilliland [États-Unis] ; S. D. Kawaler [États-Unis] ; H. Kjeldsen [Danemark] ; G. Houdek [Autriche] ; T. S. Metcalfe [États-Unis] ; J. Molenda-Zakowicz [Pologne] ; M. J. Thompson [États-Unis] ; D. A. Caldwell [États-Unis] ; J. L. Christiansen [États-Unis] ; B. Wohler [États-Unis]

Source :

RBID : Pascal:11-0466018

Descripteurs français

English descriptors

Abstract

Asteroseismology of solar-type stars has entered a new era of large surveys with the success of the NASA Kepler mission, which is providing exquisite data on oscillations of stars across the Hertzsprung-Russell diagram. From the time-series photometry, the two seismic parameters that can be most readily extracted are the large frequency separation (Δν) and the frequency of maximum oscillation power (νmax). After the survey phase, these quantities are available for hundreds of solar-type stars. By scaling from solar values, we use these two asteroseismic observables to identify for the first time an evolutionary sequence of 1 M◦. field stars, without the need for further information from stellar models. Comparison of our determinations with the few available spectroscopic results shows an excellent level of agreement. We discuss the potential of the method for differential analysis throughout the main-sequence evolution and the possibility of detecting twins of very well-known stars.
pA  
A01 01  1    @0 0004-637X
A02 01      @0 ASJOAB
A03   1    @0 Astrophys. j.
A05       @2 740
A06       @2 1 @3 p. 2
A08 01  1  ENG  @1 CONSTRUCTING A ONE-SOLAR-MASS EVOLUTIONARY SEQUENCE USING ASTEROSEISMIC DATA FROM KEPLER
A11 01  1    @1 AGUIRRE (V. Silva)
A11 02  1    @1 CHAPLIN (W. J.)
A11 03  1    @1 BALLOT (J.)
A11 04  1    @1 BASU (S.)
A11 05  1    @1 BEDDING (T. R.)
A11 06  1    @1 SERENELLI (A. M.)
A11 07  1    @1 VERNER (G. A.)
A11 08  1    @1 MIGLIO (A.)
A11 09  1    @1 MONTEIRO (M. J. P. F. G.)
A11 10  1    @1 WEISS (A.)
A11 11  1    @1 APPOURCHAUX (T.)
A11 12  1    @1 BONANNO (A.)
A11 13  1    @1 BROOMHALL (A. M.)
A11 14  1    @1 BRUNTT (H.)
A11 15  1    @1 CAMPANTE (T. L.)
A11 16  1    @1 CASAGRANDE (L.)
A11 17  1    @1 CORSARO (E.)
A11 18  1    @1 ELSWORTH (Y.)
A11 19  1    @1 GARCIA (R. A.)
A11 20  1    @1 GAULME (P.)
A11 21  1    @1 HANDBERG (R.)
A11 22  1    @1 HEKKER (S.)
A11 23  1    @1 HUBER (D.)
A11 24  1    @1 KAROFF (C.)
A11 25  1    @1 MATHUR (S.)
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A11 30  1    @1 STELLO (D.)
A11 31  1    @1 WHITE (T. R.)
A11 32  1    @1 CHRISTENSEN-DALSGAARD (J.)
A11 33  1    @1 GILLILAND (R. L.)
A11 34  1    @1 KAWALER (S. D.)
A11 35  1    @1 KJELDSEN (H.)
A11 36  1    @1 HOUDEK (G.)
A11 37  1    @1 METCALFE (T. S.)
A11 38  1    @1 MOLENDA-ZAKOWICZ (J.)
A11 39  1    @1 THOMPSON (M. J.)
A11 40  1    @1 CALDWELL (D. A.)
A11 41  1    @1 CHRISTIANSEN (J. L.)
A11 42  1    @1 WOHLER (B.)
A14 01      @1 Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str 1, 85748 @2 Garching bei München @3 DEU @Z 1 aut. @Z 10 aut. @Z 16 aut. @Z 28 aut.
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A14 03      @1 Institut de Recherche en Astrophysique et Planetologie, CNRS, 14 avenue Edouard Belin @2 31400 Toulouse @3 FRA @Z 3 aut.
A14 04      @1 Universite de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie @2 Toulouse @3 FRA @Z 3 aut.
A14 05      @1 Department of Astronomy, Yale University, P.O. Box 208101 @2 New Haven, CT 06520-8101 @3 USA @Z 4 aut.
A14 06      @1 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney @2 NSW 2006 @3 AUS @Z 5 aut. @Z 23 aut. @Z 30 aut. @Z 31 aut.
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A14 08      @1 Astronomy Unit, Queen Mary University of London @2 London, EI 4NS @3 GBR @Z 7 aut.
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A14 12      @1 Department of Physics and Astronomy, Aarhus University @2 8000 Aarhus C @3 DNK @Z 14 aut. @Z 15 aut. @Z 21 aut. @Z 24 aut. @Z 32 aut. @Z 35 aut.
A14 13      @1 Laboratoire AIM, CEA/DSM-CNRS-Universite Paris Diderot; IRFU/SAp, Centre de Saclay @2 91191 Gif-sur-Yvette @3 FRA @Z 19 aut.
A14 14      @1 Astronomical Institute "Anton Pannekoek," University of Amsterdam, Science Park 904 @2 1098 XH Amsterdam @3 NLD @Z 22 aut.
A14 15      @1 High Altitude Observatory, NCAR, P.O. Box 3000 @2 Boulder, CO 80307 @3 USA @Z 25 aut. @Z 37 aut. @Z 39 aut.
A14 16      @1 LESIA, CNRS, Universite Pierre et Marie Curie, Universite Denis Diderot, Observatoire de Paris @2 92195 Meudon @3 FRA @Z 26 aut.
A14 17      @1 Universite de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d'Azur, BP 4229 @2 06304 Nice @3 FRA @Z 27 aut.
A14 18      @1 Australian Astronomical Observatory, P.O. Box 296 @2 Epping NSW 1710 @3 AUS @Z 31 aut.
A14 19      @1 Space Telescope Science Institute, 3700 San Martin Drive @2 Baltimore, MD 21218 @3 USA @Z 33 aut.
A14 20      @1 Department of Physics and Astronomy, Iowa State University @2 Ames, IA 50014 @3 USA @Z 34 aut.
A14 21      @1 Institute of Astronomy, University of Vienna @2 1180 Vienna @3 AUT @Z 36 aut.
A14 22      @1 Instytut Astronomiczny Uniwersytetu Wroclawskiego, ul. Kopemika 11 @2 51-622 Wroclaw @3 POL @Z 38 aut.
A14 23      @1 SETI Institute/NASA Ames Research Center @2 Moffett Field, CA 94035 @3 USA @Z 40 aut. @Z 41 aut.
A14 24      @1 Orbital Sciences Corporation/NASA Ames Research Center @2 Moffett Field, CA 94035 @3 USA @Z 42 aut.
A20       @2 740L2.1-740L2.7
A21       @1 2011
A23 01      @0 ENG
A43 01      @1 INIST @2 512 @5 354000507237750020
A44       @0 0000 @1 © 2011 INIST-CNRS. All rights reserved.
A45       @0 1/4 p.
A47 01  1    @0 11-0466018
A60       @1 P
A61       @0 A
A64 01  1    @0 The Astrophysical journal
A66 01      @0 GBR
C01 01    ENG  @0 Asteroseismology of solar-type stars has entered a new era of large surveys with the success of the NASA Kepler mission, which is providing exquisite data on oscillations of stars across the Hertzsprung-Russell diagram. From the time-series photometry, the two seismic parameters that can be most readily extracted are the large frequency separation (Δν) and the frequency of maximum oscillation power (νmax). After the survey phase, these quantities are available for hundreds of solar-type stars. By scaling from solar values, we use these two asteroseismic observables to identify for the first time an evolutionary sequence of 1 M◦. field stars, without the need for further information from stellar models. Comparison of our determinations with the few available spectroscopic results shows an excellent level of agreement. We discuss the potential of the method for differential analysis throughout the main-sequence evolution and the possibility of detecting twins of very well-known stars.
C02 01  3    @0 001E03
C03 01  3  FRE  @0 Astéroséismologie @5 26
C03 01  3  ENG  @0 Astroseismology @5 26
C03 02  X  FRE  @0 Etoile type solaire @5 27
C03 02  X  ENG  @0 Solar type star @5 27
C03 02  X  SPA  @0 Estrella tipo solar @5 27
C03 03  3  FRE  @0 Série temporelle @5 28
C03 03  3  ENG  @0 Time series @5 28
C03 04  3  FRE  @0 Photométrie @5 29
C03 04  3  ENG  @0 Photometry @5 29
C03 05  3  FRE  @0 Etoile M @5 30
C03 05  3  ENG  @0 M stars @5 30
C03 06  3  FRE  @0 Modèle stellaire @5 31
C03 06  3  ENG  @0 Star models @5 31
C03 07  3  FRE  @0 Evolution stellaire @5 32
C03 07  3  ENG  @0 Stellar evolution @5 32
N21       @1 325
N44 01      @1 OTO
N82       @1 OTO

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<s1>Instytut Astronomiczny Uniwersytetu Wroclawskiego, ul. Kopemika 11</s1>
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<title xml:lang="en" level="a">CONSTRUCTING A ONE-SOLAR-MASS EVOLUTIONARY SEQUENCE USING ASTEROSEISMIC DATA FROM KEPLER</title>
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<inist:fA14 i1="04">
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<name sortKey="Garcia, R A" sort="Garcia, R A" uniqKey="Garcia R" first="R. A." last="Garcia">R. A. Garcia</name>
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<name sortKey="Gaulme, P" sort="Gaulme, P" uniqKey="Gaulme P" first="P." last="Gaulme">P. Gaulme</name>
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<s1>Institut d'Astrophysique Spatiale Universit Paris 11-CNRS (UMR8617) Batiment 121</s1>
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<name sortKey="Handberg, R" sort="Handberg, R" uniqKey="Handberg R" first="R." last="Handberg">R. Handberg</name>
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<s1>Department of Physics and Astronomy, Aarhus University</s1>
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<name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name>
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<s1>School of Physics and Astronomy, University of Birmingham</s1>
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<sZ>8 aut.</sZ>
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<country>Royaume-Uni</country>
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<inist:fA14 i1="14">
<s1>Astronomical Institute "Anton Pannekoek," University of Amsterdam, Science Park 904</s1>
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<sZ>22 aut.</sZ>
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<country>Pays-Bas</country>
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<author>
<name sortKey="Huber, D" sort="Huber, D" uniqKey="Huber D" first="D." last="Huber">D. Huber</name>
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<inist:fA14 i1="06">
<s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1>
<s2>NSW 2006</s2>
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<sZ>5 aut.</sZ>
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<country>Australie</country>
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<name sortKey="Karoff, C" sort="Karoff, C" uniqKey="Karoff C" first="C." last="Karoff">C. Karoff</name>
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<s1>Department of Physics and Astronomy, Aarhus University</s1>
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<name sortKey="Mathur, S" sort="Mathur, S" uniqKey="Mathur S" first="S." last="Mathur">S. Mathur</name>
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<inist:fA14 i1="15">
<s1>High Altitude Observatory, NCAR, P.O. Box 3000</s1>
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<name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name>
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<s1>LESIA, CNRS, Universite Pierre et Marie Curie, Universite Denis Diderot, Observatoire de Paris</s1>
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<name sortKey="Salabert, D" sort="Salabert, D" uniqKey="Salabert D" first="D." last="Salabert">D. Salabert</name>
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<inist:fA14 i1="17">
<s1>Universite de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d'Azur, BP 4229</s1>
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<author>
<name sortKey="Schonrich, R" sort="Schonrich, R" uniqKey="Schonrich R" first="R." last="Schönrich">R. Schönrich</name>
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<inist:fA14 i1="01">
<s1>Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str 1, 85748</s1>
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<sZ>1 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>28 aut.</sZ>
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<country>Allemagne</country>
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<name sortKey="Sousa, S G" sort="Sousa, S G" uniqKey="Sousa S" first="S. G." last="Sousa">S. G. Sousa</name>
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<inist:fA14 i1="09">
<s1>Centre de Astrofísica and Faculdade de Ciencias, Universidade do Porto, Rua das Estrelas</s1>
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<sZ>9 aut.</sZ>
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<country>Portugal</country>
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<author>
<name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name>
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<inist:fA14 i1="06">
<s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1>
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<sZ>5 aut.</sZ>
<sZ>23 aut.</sZ>
<sZ>30 aut.</sZ>
<sZ>31 aut.</sZ>
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<country>Australie</country>
</affiliation>
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<author>
<name sortKey="White, T R" sort="White, T R" uniqKey="White T" first="T. R." last="White">T. R. White</name>
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<inist:fA14 i1="06">
<s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1>
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<sZ>5 aut.</sZ>
<sZ>23 aut.</sZ>
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<country>Australie</country>
</affiliation>
<affiliation wicri:level="1">
<inist:fA14 i1="18">
<s1>Australian Astronomical Observatory, P.O. Box 296</s1>
<s2>Epping NSW 1710</s2>
<s3>AUS</s3>
<sZ>31 aut.</sZ>
</inist:fA14>
<country>Australie</country>
</affiliation>
</author>
<author>
<name sortKey="Christensen Dalsgaard, J" sort="Christensen Dalsgaard, J" uniqKey="Christensen Dalsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name>
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<s1>Department of Physics and Astronomy, Aarhus University</s1>
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<name sortKey="Gilliland, R L" sort="Gilliland, R L" uniqKey="Gilliland R" first="R. L." last="Gilliland">R. L. Gilliland</name>
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<inist:fA14 i1="19">
<s1>Space Telescope Science Institute, 3700 San Martin Drive</s1>
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<author>
<name sortKey="Kawaler, S D" sort="Kawaler, S D" uniqKey="Kawaler S" first="S. D." last="Kawaler">S. D. Kawaler</name>
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<inist:fA14 i1="20">
<s1>Department of Physics and Astronomy, Iowa State University</s1>
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<country>États-Unis</country>
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<name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name>
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<s1>Department of Physics and Astronomy, Aarhus University</s1>
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<sZ>15 aut.</sZ>
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<country>Danemark</country>
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<name sortKey="Houdek, G" sort="Houdek, G" uniqKey="Houdek G" first="G." last="Houdek">G. Houdek</name>
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<s1>Institute of Astronomy, University of Vienna</s1>
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<country>Autriche</country>
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<name sortKey="Metcalfe, T S" sort="Metcalfe, T S" uniqKey="Metcalfe T" first="T. S." last="Metcalfe">T. S. Metcalfe</name>
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<inist:fA14 i1="15">
<s1>High Altitude Observatory, NCAR, P.O. Box 3000</s1>
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<country>États-Unis</country>
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</author>
<author>
<name sortKey="Molenda Zakowicz, J" sort="Molenda Zakowicz, J" uniqKey="Molenda Zakowicz J" first="J." last="Molenda-Zakowicz">J. Molenda-Zakowicz</name>
<affiliation wicri:level="1">
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<s1>Instytut Astronomiczny Uniwersytetu Wroclawskiego, ul. Kopemika 11</s1>
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<s3>POL</s3>
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<country>Pologne</country>
</affiliation>
</author>
<author>
<name sortKey="Thompson, M J" sort="Thompson, M J" uniqKey="Thompson M" first="M. J." last="Thompson">M. J. Thompson</name>
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<inist:fA14 i1="15">
<s1>High Altitude Observatory, NCAR, P.O. Box 3000</s1>
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<name sortKey="Caldwell, D A" sort="Caldwell, D A" uniqKey="Caldwell D" first="D. A." last="Caldwell">D. A. Caldwell</name>
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<name sortKey="Christiansen, J L" sort="Christiansen, J L" uniqKey="Christiansen J" first="J. L." last="Christiansen">J. L. Christiansen</name>
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<name sortKey="Wohler, B" sort="Wohler, B" uniqKey="Wohler B" first="B." last="Wohler">B. Wohler</name>
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</analytic>
<series>
<title level="j" type="main">The Astrophysical journal</title>
<title level="j" type="abbreviated">Astrophys. j.</title>
<idno type="ISSN">0004-637X</idno>
<imprint>
<date when="2011">2011</date>
</imprint>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt>
<title level="j" type="main">The Astrophysical journal</title>
<title level="j" type="abbreviated">Astrophys. j.</title>
<idno type="ISSN">0004-637X</idno>
</seriesStmt>
</fileDesc>
<profileDesc>
<textClass>
<keywords scheme="KwdEn" xml:lang="en">
<term>Astroseismology</term>
<term>M stars</term>
<term>Photometry</term>
<term>Solar type star</term>
<term>Star models</term>
<term>Stellar evolution</term>
<term>Time series</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr">
<term>Astéroséismologie</term>
<term>Etoile type solaire</term>
<term>Série temporelle</term>
<term>Photométrie</term>
<term>Etoile M</term>
<term>Modèle stellaire</term>
<term>Evolution stellaire</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front>
<div type="abstract" xml:lang="en">Asteroseismology of solar-type stars has entered a new era of large surveys with the success of the NASA Kepler mission, which is providing exquisite data on oscillations of stars across the Hertzsprung-Russell diagram. From the time-series photometry, the two seismic parameters that can be most readily extracted are the large frequency separation (Δν) and the frequency of maximum oscillation power (ν
<sub>max</sub>
). After the survey phase, these quantities are available for hundreds of solar-type stars. By scaling from solar values, we use these two asteroseismic observables to identify for the first time an evolutionary sequence of 1 M
<sub>◦.</sub>
field stars, without the need for further information from stellar models. Comparison of our determinations with the few available spectroscopic results shows an excellent level of agreement. We discuss the potential of the method for differential analysis throughout the main-sequence evolution and the possibility of detecting twins of very well-known stars.</div>
</front>
</TEI>
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<s1>CONSTRUCTING A ONE-SOLAR-MASS EVOLUTIONARY SEQUENCE USING ASTEROSEISMIC DATA FROM KEPLER</s1>
</fA08>
<fA11 i1="01" i2="1">
<s1>AGUIRRE (V. Silva)</s1>
</fA11>
<fA11 i1="02" i2="1">
<s1>CHAPLIN (W. J.)</s1>
</fA11>
<fA11 i1="03" i2="1">
<s1>BALLOT (J.)</s1>
</fA11>
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<s1>BASU (S.)</s1>
</fA11>
<fA11 i1="05" i2="1">
<s1>BEDDING (T. R.)</s1>
</fA11>
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<s1>SERENELLI (A. M.)</s1>
</fA11>
<fA11 i1="07" i2="1">
<s1>VERNER (G. A.)</s1>
</fA11>
<fA11 i1="08" i2="1">
<s1>MIGLIO (A.)</s1>
</fA11>
<fA11 i1="09" i2="1">
<s1>MONTEIRO (M. J. P. F. G.)</s1>
</fA11>
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<s1>WEISS (A.)</s1>
</fA11>
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<s1>APPOURCHAUX (T.)</s1>
</fA11>
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<s1>BONANNO (A.)</s1>
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<s1>BROOMHALL (A. M.)</s1>
</fA11>
<fA11 i1="14" i2="1">
<s1>BRUNTT (H.)</s1>
</fA11>
<fA11 i1="15" i2="1">
<s1>CAMPANTE (T. L.)</s1>
</fA11>
<fA11 i1="16" i2="1">
<s1>CASAGRANDE (L.)</s1>
</fA11>
<fA11 i1="17" i2="1">
<s1>CORSARO (E.)</s1>
</fA11>
<fA11 i1="18" i2="1">
<s1>ELSWORTH (Y.)</s1>
</fA11>
<fA11 i1="19" i2="1">
<s1>GARCIA (R. A.)</s1>
</fA11>
<fA11 i1="20" i2="1">
<s1>GAULME (P.)</s1>
</fA11>
<fA11 i1="21" i2="1">
<s1>HANDBERG (R.)</s1>
</fA11>
<fA11 i1="22" i2="1">
<s1>HEKKER (S.)</s1>
</fA11>
<fA11 i1="23" i2="1">
<s1>HUBER (D.)</s1>
</fA11>
<fA11 i1="24" i2="1">
<s1>KAROFF (C.)</s1>
</fA11>
<fA11 i1="25" i2="1">
<s1>MATHUR (S.)</s1>
</fA11>
<fA11 i1="26" i2="1">
<s1>MOSSER (B.)</s1>
</fA11>
<fA11 i1="27" i2="1">
<s1>SALABERT (D.)</s1>
</fA11>
<fA11 i1="28" i2="1">
<s1>SCHÖNRICH (R.)</s1>
</fA11>
<fA11 i1="29" i2="1">
<s1>SOUSA (S. G.)</s1>
</fA11>
<fA11 i1="30" i2="1">
<s1>STELLO (D.)</s1>
</fA11>
<fA11 i1="31" i2="1">
<s1>WHITE (T. R.)</s1>
</fA11>
<fA11 i1="32" i2="1">
<s1>CHRISTENSEN-DALSGAARD (J.)</s1>
</fA11>
<fA11 i1="33" i2="1">
<s1>GILLILAND (R. L.)</s1>
</fA11>
<fA11 i1="34" i2="1">
<s1>KAWALER (S. D.)</s1>
</fA11>
<fA11 i1="35" i2="1">
<s1>KJELDSEN (H.)</s1>
</fA11>
<fA11 i1="36" i2="1">
<s1>HOUDEK (G.)</s1>
</fA11>
<fA11 i1="37" i2="1">
<s1>METCALFE (T. S.)</s1>
</fA11>
<fA11 i1="38" i2="1">
<s1>MOLENDA-ZAKOWICZ (J.)</s1>
</fA11>
<fA11 i1="39" i2="1">
<s1>THOMPSON (M. J.)</s1>
</fA11>
<fA11 i1="40" i2="1">
<s1>CALDWELL (D. A.)</s1>
</fA11>
<fA11 i1="41" i2="1">
<s1>CHRISTIANSEN (J. L.)</s1>
</fA11>
<fA11 i1="42" i2="1">
<s1>WOHLER (B.)</s1>
</fA11>
<fA14 i1="01">
<s1>Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str 1, 85748</s1>
<s2>Garching bei München</s2>
<s3>DEU</s3>
<sZ>1 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>28 aut.</sZ>
</fA14>
<fA14 i1="02">
<s1>School of Physics and Astronomy, University of Birmingham</s1>
<s2>Birmingham, B 15 2TT</s2>
<s3>GBR</s3>
<sZ>2 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>13 aut.</sZ>
<sZ>18 aut.</sZ>
<sZ>22 aut.</sZ>
</fA14>
<fA14 i1="03">
<s1>Institut de Recherche en Astrophysique et Planetologie, CNRS, 14 avenue Edouard Belin</s1>
<s2>31400 Toulouse</s2>
<s3>FRA</s3>
<sZ>3 aut.</sZ>
</fA14>
<fA14 i1="04">
<s1>Universite de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie</s1>
<s2>Toulouse</s2>
<s3>FRA</s3>
<sZ>3 aut.</sZ>
</fA14>
<fA14 i1="05">
<s1>Department of Astronomy, Yale University, P.O. Box 208101</s1>
<s2>New Haven, CT 06520-8101</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
</fA14>
<fA14 i1="06">
<s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1>
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<s3>AUS</s3>
<sZ>5 aut.</sZ>
<sZ>23 aut.</sZ>
<sZ>30 aut.</sZ>
<sZ>31 aut.</sZ>
</fA14>
<fA14 i1="07">
<s1>Instituto de Ciencias del Espacio (CSIC-IEEC), Facultad de Ciències, Campus UAB</s1>
<s2>08193 Bellaterra</s2>
<s3>ESP</s3>
<sZ>6 aut.</sZ>
</fA14>
<fA14 i1="08">
<s1>Astronomy Unit, Queen Mary University of London</s1>
<s2>London, EI 4NS</s2>
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<sZ>7 aut.</sZ>
</fA14>
<fA14 i1="09">
<s1>Centre de Astrofísica and Faculdade de Ciencias, Universidade do Porto, Rua das Estrelas</s1>
<s2>4150-762 Porto</s2>
<s3>PRT</s3>
<sZ>9 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>29 aut.</sZ>
</fA14>
<fA14 i1="10">
<s1>Institut d'Astrophysique Spatiale Universit Paris 11-CNRS (UMR8617) Batiment 121</s1>
<s2>91405 ORSAY</s2>
<s3>FRA</s3>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</fA14>
<fA14 i1="11">
<s1>INAF-Osservatorio Astrofisico di Catania, Via S. Sofia 78</s1>
<s2>95123 Catania</s2>
<s3>ITA</s3>
<sZ>12 aut.</sZ>
<sZ>17 aut.</sZ>
</fA14>
<fA14 i1="12">
<s1>Department of Physics and Astronomy, Aarhus University</s1>
<s2>8000 Aarhus C</s2>
<s3>DNK</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>21 aut.</sZ>
<sZ>24 aut.</sZ>
<sZ>32 aut.</sZ>
<sZ>35 aut.</sZ>
</fA14>
<fA14 i1="13">
<s1>Laboratoire AIM, CEA/DSM-CNRS-Universite Paris Diderot; IRFU/SAp, Centre de Saclay</s1>
<s2>91191 Gif-sur-Yvette</s2>
<s3>FRA</s3>
<sZ>19 aut.</sZ>
</fA14>
<fA14 i1="14">
<s1>Astronomical Institute "Anton Pannekoek," University of Amsterdam, Science Park 904</s1>
<s2>1098 XH Amsterdam</s2>
<s3>NLD</s3>
<sZ>22 aut.</sZ>
</fA14>
<fA14 i1="15">
<s1>High Altitude Observatory, NCAR, P.O. Box 3000</s1>
<s2>Boulder, CO 80307</s2>
<s3>USA</s3>
<sZ>25 aut.</sZ>
<sZ>37 aut.</sZ>
<sZ>39 aut.</sZ>
</fA14>
<fA14 i1="16">
<s1>LESIA, CNRS, Universite Pierre et Marie Curie, Universite Denis Diderot, Observatoire de Paris</s1>
<s2>92195 Meudon</s2>
<s3>FRA</s3>
<sZ>26 aut.</sZ>
</fA14>
<fA14 i1="17">
<s1>Universite de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d'Azur, BP 4229</s1>
<s2>06304 Nice</s2>
<s3>FRA</s3>
<sZ>27 aut.</sZ>
</fA14>
<fA14 i1="18">
<s1>Australian Astronomical Observatory, P.O. Box 296</s1>
<s2>Epping NSW 1710</s2>
<s3>AUS</s3>
<sZ>31 aut.</sZ>
</fA14>
<fA14 i1="19">
<s1>Space Telescope Science Institute, 3700 San Martin Drive</s1>
<s2>Baltimore, MD 21218</s2>
<s3>USA</s3>
<sZ>33 aut.</sZ>
</fA14>
<fA14 i1="20">
<s1>Department of Physics and Astronomy, Iowa State University</s1>
<s2>Ames, IA 50014</s2>
<s3>USA</s3>
<sZ>34 aut.</sZ>
</fA14>
<fA14 i1="21">
<s1>Institute of Astronomy, University of Vienna</s1>
<s2>1180 Vienna</s2>
<s3>AUT</s3>
<sZ>36 aut.</sZ>
</fA14>
<fA14 i1="22">
<s1>Instytut Astronomiczny Uniwersytetu Wroclawskiego, ul. Kopemika 11</s1>
<s2>51-622 Wroclaw</s2>
<s3>POL</s3>
<sZ>38 aut.</sZ>
</fA14>
<fA14 i1="23">
<s1>SETI Institute/NASA Ames Research Center</s1>
<s2>Moffett Field, CA 94035</s2>
<s3>USA</s3>
<sZ>40 aut.</sZ>
<sZ>41 aut.</sZ>
</fA14>
<fA14 i1="24">
<s1>Orbital Sciences Corporation/NASA Ames Research Center</s1>
<s2>Moffett Field, CA 94035</s2>
<s3>USA</s3>
<sZ>42 aut.</sZ>
</fA14>
<fA20>
<s2>740L2.1-740L2.7</s2>
</fA20>
<fA21>
<s1>2011</s1>
</fA21>
<fA23 i1="01">
<s0>ENG</s0>
</fA23>
<fA43 i1="01">
<s1>INIST</s1>
<s2>512</s2>
<s5>354000507237750020</s5>
</fA43>
<fA44>
<s0>0000</s0>
<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45>
<s0>1/4 p.</s0>
</fA45>
<fA47 i1="01" i2="1">
<s0>11-0466018</s0>
</fA47>
<fA60>
<s1>P</s1>
</fA60>
<fA61>
<s0>A</s0>
</fA61>
<fA64 i1="01" i2="1">
<s0>The Astrophysical journal</s0>
</fA64>
<fA66 i1="01">
<s0>GBR</s0>
</fA66>
<fC01 i1="01" l="ENG">
<s0>Asteroseismology of solar-type stars has entered a new era of large surveys with the success of the NASA Kepler mission, which is providing exquisite data on oscillations of stars across the Hertzsprung-Russell diagram. From the time-series photometry, the two seismic parameters that can be most readily extracted are the large frequency separation (Δν) and the frequency of maximum oscillation power (ν
<sub>max</sub>
). After the survey phase, these quantities are available for hundreds of solar-type stars. By scaling from solar values, we use these two asteroseismic observables to identify for the first time an evolutionary sequence of 1 M
<sub>◦.</sub>
field stars, without the need for further information from stellar models. Comparison of our determinations with the few available spectroscopic results shows an excellent level of agreement. We discuss the potential of the method for differential analysis throughout the main-sequence evolution and the possibility of detecting twins of very well-known stars.</s0>
</fC01>
<fC02 i1="01" i2="3">
<s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE">
<s0>Astéroséismologie</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG">
<s0>Astroseismology</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="X" l="FRE">
<s0>Etoile type solaire</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="ENG">
<s0>Solar type star</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="SPA">
<s0>Estrella tipo solar</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="3" l="FRE">
<s0>Série temporelle</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="3" l="ENG">
<s0>Time series</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="3" l="FRE">
<s0>Photométrie</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="3" l="ENG">
<s0>Photometry</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE">
<s0>Etoile M</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG">
<s0>M stars</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE">
<s0>Modèle stellaire</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG">
<s0>Star models</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE">
<s0>Evolution stellaire</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG">
<s0>Stellar evolution</s0>
<s5>32</s5>
</fC03>
<fN21>
<s1>325</s1>
</fN21>
<fN44 i1="01">
<s1>OTO</s1>
</fN44>
<fN82>
<s1>OTO</s1>
</fN82>
</pA>
</standard>
</inist>
</record>

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