VERIFYING ASTEROSEISMICALLY DETERMINED PARAMETERS OF KEPLER STARS USING HIPPARCOS PARALLAXES: SELF-CONSISTENT STELLAR PROPERTIES AND DISTANCES
Identifieur interne : 004F49 ( PascalFrancis/Curation ); précédent : 004F48; suivant : 004F50VERIFYING ASTEROSEISMICALLY DETERMINED PARAMETERS OF KEPLER STARS USING HIPPARCOS PARALLAXES: SELF-CONSISTENT STELLAR PROPERTIES AND DISTANCES
Auteurs : V. Silva Aguirre [Danemark, Allemagne, États-Unis] ; L. Casagrande [Australie] ; S. Basu [États-Unis] ; T. L. Campante [Portugal, Royaume-Uni] ; W. J. Chaplin [Danemark, États-Unis, Royaume-Uni] ; D. Huber [États-Unis] ; A. Miglio [Royaume-Uni] ; A. M. Serenelli [États-Unis, Espagne] ; J. Ballot [France] ; T. R. Bedding [Danemark, Australie] ; J. Christensen-Dalsgaard [Danemark, États-Unis] ; O. L. Creevey [France] ; Y. Elsworth [Royaume-Uni] ; R. A. Garcia [États-Unis, France] ; R. L. Gilliland [États-Unis] ; S. Hekker [Royaume-Uni, Pays-Bas] ; H. Kjeldsen [Danemark] ; S. Mathur [États-Unis] ; T. S. Metcalfe [États-Unis] ; M. J. P. F. G. Monteiro [Portugal] ; B. Mosser [France] ; M. H. Pinsonneault [États-Unis] ; D. Stello [Australie] ; A. Weiss [Allemagne] ; P. Tenenbaum [États-Unis] ; J. D. Twicken [États-Unis] ; K. Uddin [États-Unis]Source :
- The Astrophysical journal [ 0004-637X ] ; 2012.
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Abstract
Accurately determining the properties of stars is of prime importance for characterizing stellar populations in our Galaxy. The field of asteroseismology has been thought to be particularly successful in such an endeavor for stars in different evolutionary stages. However, to fully exploit its potential, robust methods for estimating stellar parameters are required and independent verification of the results is mandatory. With this purpose, we present a new technique to obtain stellar properties by coupling asteroseismic analysis with the InfraRed Flux Method. By using two global seismic observables and multi-band photometry, the technique allows us to obtain masses, radii, effective temperatures, bolometric fluxes, and hence distances for field stars in a self-consistent manner. We apply our method to 22 solar-like oscillators in the Kepler short-cadence sample, that have accurate Hipparcos parallaxes. Our distance determinations agree to better than 5%, while measurements of spectroscopic effective temperatures and interferometric radii also validate our results. We briefly discuss the potential of our technique for stellar population analysis and models of Galactic Chemical Evolution.
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University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Huber, D" sort="Huber, D" uniqKey="Huber D" first="D." last="Huber">D. Huber</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>6 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Miglio, A" sort="Miglio, A" uniqKey="Miglio A" first="A." last="Miglio">A. Miglio</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>School of Physics and Astronomy. University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Serenelli, A M" sort="Serenelli, A M" uniqKey="Serenelli A" first="A. M." last="Serenelli">A. M. 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Ballot</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 avenue Edouard Belin</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>9 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>University de Toulouse, UPS-OMP, IRAP</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>9 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Bedding, T R" sort="Bedding, T R" uniqKey="Bedding T" first="T. R." last="Bedding">T. R. Bedding</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>Danemark</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006</s1><s3>AUS</s3><sZ>10 aut.</sZ><sZ>23 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><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>Danemark</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Creevey, O L" sort="Creevey, O L" uniqKey="Creevey O" first="O. L." last="Creevey">O. L. Creevey</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Laboratoire Lagrange, UMR 7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte dAzur</s1><s2>06304 Nice</s2><s3>FRA</s3><sZ>12 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Elsworth, Y" sort="Elsworth, Y" uniqKey="Elsworth Y" first="Y." last="Elsworth">Y. Elsworth</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>School of Physics and Astronomy. University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Garcia, R A" sort="Garcia, R A" uniqKey="Garcia R" first="R. A." last="Garcia">R. A. Garcia</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot. IRFU/SAp, Centre de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>14 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Gilliland, R L" sort="Gilliland, R L" uniqKey="Gilliland R" first="R. L." last="Gilliland">R. L. Gilliland</name><affiliation wicri:level="1"><inist:fA14 i1="15"><s1>Center for Exoplanets and Habitable Worlds, The Pennsylvania State University</s1><s2>University Park, PA</s2><s3>USA</s3><sZ>15 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>School of Physics and Astronomy. University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="16"><s1>Astronomical Institute "Anton Pannekoek," University of Amsterdam, Science Park 904</s1><s2>1098 XH Amsterdam</s2><s3>NLD</s3><sZ>16 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Mathur, S" sort="Mathur, S" uniqKey="Mathur S" first="S." last="Mathur">S. Mathur</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="17"><s1>High Altitude Observatory, NCAR, P.O. Box 3000</s1><s2>Boulder, CO 80307</s2><s3>USA</s3><sZ>18 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Metcalfe, T S" sort="Metcalfe, T S" uniqKey="Metcalfe T" first="T. S." last="Metcalfe">T. S. Metcalfe</name><affiliation wicri:level="1"><inist:fA14 i1="18"><s1>Space Science Institute</s1><s2>Boulder, CO 80301</s2><s3>USA</s3><sZ>19 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Monteiro, M J P F G" sort="Monteiro, M J P F G" uniqKey="Monteiro M" first="M. J. P. F. G." last="Monteiro">M. J. P. F. G. Monteiro</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Centro de Astrofísica and Faculdade de Ciências, Universidade do Porto, Rua das Estrelas</s1><s2>4150-762 Porto</s2><s3>PRT</s3><sZ>4 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>Portugal</country></affiliation></author><author><name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name><affiliation wicri:level="1"><inist:fA14 i1="19"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>21 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Pinsonneault, M H" sort="Pinsonneault, M H" uniqKey="Pinsonneault M" first="M. H." last="Pinsonneault">M. H. Pinsonneault</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="20"><s1>Department of Astronomy, The Ohio State University</s1><s2>Columbus, OH 43210</s2><s3>USA</s3><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006</s1><s3>AUS</s3><sZ>10 aut.</sZ><sZ>23 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Weiss, A" sort="Weiss, A" uniqKey="Weiss A" first="A." last="Weiss">A. Weiss</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Max Planck Institute for Astrophysics. Karl-Schwarzschild-Str. 1</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>24 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Tenenbaum, P" sort="Tenenbaum, P" uniqKey="Tenenbaum P" first="P." last="Tenenbaum">P. Tenenbaum</name><affiliation wicri:level="1"><inist:fA14 i1="21"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffett Field. CA 94035</s2><s3>USA</s3><sZ>25 aut.</sZ><sZ>26 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Twicken, J D" sort="Twicken, J D" uniqKey="Twicken J" first="J. D." last="Twicken">J. D. Twicken</name><affiliation wicri:level="1"><inist:fA14 i1="21"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffett Field. CA 94035</s2><s3>USA</s3><sZ>25 aut.</sZ><sZ>26 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Uddin, K" sort="Uddin, K" uniqKey="Uddin K" first="K." last="Uddin">K. Uddin</name><affiliation wicri:level="1"><inist:fA14 i1="22"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>27 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">12-0384691</idno><date when="2012">2012</date><idno type="stanalyst">PASCAL 12-0384691 INIST</idno><idno type="RBID">Pascal:12-0384691</idno><idno type="wicri:Area/PascalFrancis/Corpus">000F69</idno><idno type="wicri:Area/PascalFrancis/Curation">004F49</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">VERIFYING ASTEROSEISMICALLY DETERMINED PARAMETERS OF KEPLER STARS USING HIPPARCOS PARALLAXES: SELF-CONSISTENT STELLAR PROPERTIES AND DISTANCES</title><author><name sortKey="Silva Aguirre, V" sort="Silva Aguirre, V" uniqKey="Silva Aguirre V" first="V." last="Silva Aguirre">V. Silva Aguirre</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>Danemark</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Max Planck Institute for Astrophysics. Karl-Schwarzschild-Str. 1</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>24 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Casagrande, L" sort="Casagrande, L" uniqKey="Casagrande L" first="L." last="Casagrande">L. Casagrande</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University. ACT 261</s1><s3>AUS</s3><sZ>2 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Basu, S" sort="Basu, S" uniqKey="Basu S" first="S." last="Basu">S. Basu</name><affiliation wicri:level="1"><inist: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>3 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Campante, T L" sort="Campante, T L" uniqKey="Campante T" first="T. L." last="Campante">T. L. Campante</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Centro de Astrofísica and Faculdade de Ciências, Universidade do Porto, Rua das Estrelas</s1><s2>4150-762 Porto</s2><s3>PRT</s3><sZ>4 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>Portugal</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>School of Physics and Astronomy. University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Chaplin, W J" sort="Chaplin, W J" uniqKey="Chaplin W" first="W. J." last="Chaplin">W. J. Chaplin</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>Danemark</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>School of Physics and Astronomy. University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Huber, D" sort="Huber, D" uniqKey="Huber D" first="D." last="Huber">D. Huber</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>6 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Miglio, A" sort="Miglio, A" uniqKey="Miglio A" first="A." last="Miglio">A. Miglio</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>School of Physics and Astronomy. University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Serenelli, A M" sort="Serenelli, A M" uniqKey="Serenelli A" first="A. M." last="Serenelli">A. M. Serenelli</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Instituto de Ciencias del Espacio (CSIC-IEEC), Facultad de Ciències, Campus UAB</s1><s2>08193 Bellaterra</s2><s3>ESP</s3><sZ>8 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Ballot, J" sort="Ballot, J" uniqKey="Ballot J" first="J." last="Ballot">J. Ballot</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 avenue Edouard Belin</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>9 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>University de Toulouse, UPS-OMP, IRAP</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>9 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Bedding, T R" sort="Bedding, T R" uniqKey="Bedding T" first="T. R." last="Bedding">T. R. Bedding</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>Danemark</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006</s1><s3>AUS</s3><sZ>10 aut.</sZ><sZ>23 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><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>Danemark</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Creevey, O L" sort="Creevey, O L" uniqKey="Creevey O" first="O. L." last="Creevey">O. L. Creevey</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Laboratoire Lagrange, UMR 7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte dAzur</s1><s2>06304 Nice</s2><s3>FRA</s3><sZ>12 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Elsworth, Y" sort="Elsworth, Y" uniqKey="Elsworth Y" first="Y." last="Elsworth">Y. Elsworth</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>School of Physics and Astronomy. University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Garcia, R A" sort="Garcia, R A" uniqKey="Garcia R" first="R. A." last="Garcia">R. A. Garcia</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot. IRFU/SAp, Centre de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>14 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Gilliland, R L" sort="Gilliland, R L" uniqKey="Gilliland R" first="R. L." last="Gilliland">R. L. Gilliland</name><affiliation wicri:level="1"><inist:fA14 i1="15"><s1>Center for Exoplanets and Habitable Worlds, The Pennsylvania State University</s1><s2>University Park, PA</s2><s3>USA</s3><sZ>15 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>School of Physics and Astronomy. University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="16"><s1>Astronomical Institute "Anton Pannekoek," University of Amsterdam, Science Park 904</s1><s2>1098 XH Amsterdam</s2><s3>NLD</s3><sZ>16 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>17 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Mathur, S" sort="Mathur, S" uniqKey="Mathur S" first="S." last="Mathur">S. Mathur</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="17"><s1>High Altitude Observatory, NCAR, P.O. Box 3000</s1><s2>Boulder, CO 80307</s2><s3>USA</s3><sZ>18 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Metcalfe, T S" sort="Metcalfe, T S" uniqKey="Metcalfe T" first="T. S." last="Metcalfe">T. S. Metcalfe</name><affiliation wicri:level="1"><inist:fA14 i1="18"><s1>Space Science Institute</s1><s2>Boulder, CO 80301</s2><s3>USA</s3><sZ>19 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Monteiro, M J P F G" sort="Monteiro, M J P F G" uniqKey="Monteiro M" first="M. J. P. F. G." last="Monteiro">M. J. P. F. G. Monteiro</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Centro de Astrofísica and Faculdade de Ciências, Universidade do Porto, Rua das Estrelas</s1><s2>4150-762 Porto</s2><s3>PRT</s3><sZ>4 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>Portugal</country></affiliation></author><author><name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name><affiliation wicri:level="1"><inist:fA14 i1="19"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>21 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Pinsonneault, M H" sort="Pinsonneault, M H" uniqKey="Pinsonneault M" first="M. H." last="Pinsonneault">M. H. Pinsonneault</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="20"><s1>Department of Astronomy, The Ohio State University</s1><s2>Columbus, OH 43210</s2><s3>USA</s3><sZ>22 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006</s1><s3>AUS</s3><sZ>10 aut.</sZ><sZ>23 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Weiss, A" sort="Weiss, A" uniqKey="Weiss A" first="A." last="Weiss">A. Weiss</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Max Planck Institute for Astrophysics. Karl-Schwarzschild-Str. 1</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>24 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Tenenbaum, P" sort="Tenenbaum, P" uniqKey="Tenenbaum P" first="P." last="Tenenbaum">P. Tenenbaum</name><affiliation wicri:level="1"><inist:fA14 i1="21"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffett Field. CA 94035</s2><s3>USA</s3><sZ>25 aut.</sZ><sZ>26 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Twicken, J D" sort="Twicken, J D" uniqKey="Twicken J" first="J. D." last="Twicken">J. D. Twicken</name><affiliation wicri:level="1"><inist:fA14 i1="21"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffett Field. CA 94035</s2><s3>USA</s3><sZ>25 aut.</sZ><sZ>26 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Uddin, K" sort="Uddin, K" uniqKey="Uddin K" first="K." last="Uddin">K. Uddin</name><affiliation wicri:level="1"><inist:fA14 i1="22"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>27 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author></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="2012">2012</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>Chemical evolution</term><term>Distance measurement</term><term>Effective mass</term><term>Effective radius</term><term>Effective temperature</term><term>Galactic evolution</term><term>Galaxies</term><term>Milky Way</term><term>Models</term><term>Oscillators</term><term>Photometry</term><term>Physical parameter</term><term>Stellar population</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Population stellaire</term><term>Galaxies</term><term>Astéroséismologie</term><term>Paramètre physique</term><term>Photométrie</term><term>Masse effective</term><term>Rayon effectif</term><term>Oscillateur</term><term>Mesure distance</term><term>Température effective</term><term>Modèle</term><term>Evolution galactique</term><term>Evolution chimique</term><term>Voie lactée</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Accurately determining the properties of stars is of prime importance for characterizing stellar populations in our Galaxy. The field of asteroseismology has been thought to be particularly successful in such an endeavor for stars in different evolutionary stages. However, to fully exploit its potential, robust methods for estimating stellar parameters are required and independent verification of the results is mandatory. With this purpose, we present a new technique to obtain stellar properties by coupling asteroseismic analysis with the InfraRed Flux Method. By using two global seismic observables and multi-band photometry, the technique allows us to obtain masses, radii, effective temperatures, bolometric fluxes, and hence distances for field stars in a self-consistent manner. We apply our method to 22 solar-like oscillators in the Kepler short-cadence sample, that have accurate Hipparcos parallaxes. Our distance determinations agree to better than 5%, while measurements of spectroscopic effective temperatures and interferometric radii also validate our results. We briefly discuss the potential of our technique for stellar population analysis and models of Galactic Chemical Evolution.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-637X</s0></fA01><fA02 i1="01"><s0>ASJOAB</s0></fA02><fA03 i2="1"><s0>Astrophys. j.</s0></fA03><fA05><s2>757</s2></fA05><fA06><s2>1</s2><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>VERIFYING ASTEROSEISMICALLY DETERMINED PARAMETERS OF KEPLER STARS USING HIPPARCOS PARALLAXES: SELF-CONSISTENT STELLAR PROPERTIES AND DISTANCES</s1></fA08><fA11 i1="01" i2="1"><s1>SILVA AGUIRRE (V.)</s1></fA11><fA11 i1="02" i2="1"><s1>CASAGRANDE (L.)</s1></fA11><fA11 i1="03" i2="1"><s1>BASU (S.)</s1></fA11><fA11 i1="04" i2="1"><s1>CAMPANTE (T. L.)</s1></fA11><fA11 i1="05" i2="1"><s1>CHAPLIN (W. J.)</s1></fA11><fA11 i1="06" i2="1"><s1>HUBER (D.)</s1></fA11><fA11 i1="07" i2="1"><s1>MIGLIO (A.)</s1></fA11><fA11 i1="08" i2="1"><s1>SERENELLI (A. M.)</s1></fA11><fA11 i1="09" i2="1"><s1>BALLOT (J.)</s1></fA11><fA11 i1="10" i2="1"><s1>BEDDING (T. R.)</s1></fA11><fA11 i1="11" i2="1"><s1>CHRISTENSEN-DALSGAARD (J.)</s1></fA11><fA11 i1="12" i2="1"><s1>CREEVEY (O. L.)</s1></fA11><fA11 i1="13" i2="1"><s1>ELSWORTH (Y.)</s1></fA11><fA11 i1="14" i2="1"><s1>GARCIA (R. A.)</s1></fA11><fA11 i1="15" i2="1"><s1>GILLILAND (R. L.)</s1></fA11><fA11 i1="16" i2="1"><s1>HEKKER (S.)</s1></fA11><fA11 i1="17" i2="1"><s1>KJELDSEN (H.)</s1></fA11><fA11 i1="18" i2="1"><s1>MATHUR (S.)</s1></fA11><fA11 i1="19" i2="1"><s1>METCALFE (T. S.)</s1></fA11><fA11 i1="20" i2="1"><s1>MONTEIRO (M. J. P. F. G.)</s1></fA11><fA11 i1="21" i2="1"><s1>MOSSER (B.)</s1></fA11><fA11 i1="22" i2="1"><s1>PINSONNEAULT (M. H.)</s1></fA11><fA11 i1="23" i2="1"><s1>STELLO (D.)</s1></fA11><fA11 i1="24" i2="1"><s1>WEISS (A.)</s1></fA11><fA11 i1="25" i2="1"><s1>TENENBAUM (P.)</s1></fA11><fA11 i1="26" i2="1"><s1>TWICKEN (J. D.)</s1></fA11><fA11 i1="27" i2="1"><s1>UDDIN (K.)</s1></fA11><fA14 i1="01"><s1>Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>17 aut.</sZ></fA14><fA14 i1="02"><s1>Max Planck Institute for Astrophysics. Karl-Schwarzschild-Str. 1</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>24 aut.</sZ></fA14><fA14 i1="03"><s1>Kavli Institute for Theoretical Physics</s1><s2>Santa Barbara, CA 93106</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>8 aut.</sZ><sZ>11 aut.</sZ><sZ>14 aut.</sZ><sZ>18 aut.</sZ><sZ>22 aut.</sZ></fA14><fA14 i1="04"><s1>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University. ACT 261</s1><s3>AUS</s3><sZ>2 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>3 aut.</sZ></fA14><fA14 i1="06"><s1>Centro de Astrofísica and Faculdade de Ciências, Universidade do Porto, Rua das Estrelas</s1><s2>4150-762 Porto</s2><s3>PRT</s3><sZ>4 aut.</sZ><sZ>20 aut.</sZ></fA14><fA14 i1="07"><s1>School of Physics and Astronomy. University of Birmingham</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>13 aut.</sZ><sZ>16 aut.</sZ></fA14><fA14 i1="08"><s1>NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>6 aut.</sZ></fA14><fA14 i1="09"><s1>Instituto de Ciencias del Espacio (CSIC-IEEC), Facultad de Ciències, Campus UAB</s1><s2>08193 Bellaterra</s2><s3>ESP</s3><sZ>8 aut.</sZ></fA14><fA14 i1="10"><s1>CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 avenue Edouard Belin</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>9 aut.</sZ></fA14><fA14 i1="11"><s1>University de Toulouse, UPS-OMP, IRAP</s1><s2>31400 Toulouse</s2><s3>FRA</s3><sZ>9 aut.</sZ></fA14><fA14 i1="12"><s1>Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006</s1><s3>AUS</s3><sZ>10 aut.</sZ><sZ>23 aut.</sZ></fA14><fA14 i1="13"><s1>Laboratoire Lagrange, UMR 7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte dAzur</s1><s2>06304 Nice</s2><s3>FRA</s3><sZ>12 aut.</sZ></fA14><fA14 i1="14"><s1>Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot. IRFU/SAp, Centre de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>14 aut.</sZ></fA14><fA14 i1="15"><s1>Center for Exoplanets and Habitable Worlds, The Pennsylvania State University</s1><s2>University Park, PA</s2><s3>USA</s3><sZ>15 aut.</sZ></fA14><fA14 i1="16"><s1>Astronomical Institute "Anton Pannekoek," University of Amsterdam, Science Park 904</s1><s2>1098 XH Amsterdam</s2><s3>NLD</s3><sZ>16 aut.</sZ></fA14><fA14 i1="17"><s1>High Altitude Observatory, NCAR, P.O. Box 3000</s1><s2>Boulder, CO 80307</s2><s3>USA</s3><sZ>18 aut.</sZ></fA14><fA14 i1="18"><s1>Space Science Institute</s1><s2>Boulder, CO 80301</s2><s3>USA</s3><sZ>19 aut.</sZ></fA14><fA14 i1="19"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>21 aut.</sZ></fA14><fA14 i1="20"><s1>Department of Astronomy, The Ohio State University</s1><s2>Columbus, OH 43210</s2><s3>USA</s3><sZ>22 aut.</sZ></fA14><fA14 i1="21"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffett Field. CA 94035</s2><s3>USA</s3><sZ>25 aut.</sZ><sZ>26 aut.</sZ></fA14><fA14 i1="22"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>27 aut.</sZ></fA14><fA20><s2>99.1-99.11</s2></fA20><fA21><s1>2012</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>512</s2><s5>354000505313840990</s5></fA43><fA44><s0>0000</s0><s1>© 2012 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1 p.</s0></fA45><fA47 i1="01" i2="1"><s0>12-0384691</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>Accurately determining the properties of stars is of prime importance for characterizing stellar populations in our Galaxy. The field of asteroseismology has been thought to be particularly successful in such an endeavor for stars in different evolutionary stages. However, to fully exploit its potential, robust methods for estimating stellar parameters are required and independent verification of the results is mandatory. With this purpose, we present a new technique to obtain stellar properties by coupling asteroseismic analysis with the InfraRed Flux Method. By using two global seismic observables and multi-band photometry, the technique allows us to obtain masses, radii, effective temperatures, bolometric fluxes, and hence distances for field stars in a self-consistent manner. We apply our method to 22 solar-like oscillators in the Kepler short-cadence sample, that have accurate Hipparcos parallaxes. Our distance determinations agree to better than 5%, while measurements of spectroscopic effective temperatures and interferometric radii also validate our results. We briefly discuss the potential of our technique for stellar population analysis and models of Galactic Chemical Evolution.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Population stellaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Stellar population</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Población estelar</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Galaxies</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Galaxies</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Astéroséismologie</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Astroseismology</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Paramètre physique</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Physical parameter</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Parámetro físico</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Photométrie</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Photometry</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Masse effective</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Effective mass</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Rayon effectif</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Effective radius</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Radio efectivo</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Oscillateur</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Oscillators</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Mesure distance</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Distance measurement</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Température effective</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Effective temperature</s0><s5>35</s5></fC03><fC03 i1="11" i2="X" l="FRE"><s0>Modèle</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="ENG"><s0>Models</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="SPA"><s0>Modelo</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Evolution galactique</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Galactic evolution</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Evolution chimique</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Chemical evolution</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Evolución química</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Voie lactée</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Milky Way</s0><s5>39</s5></fC03><fN21><s1>296</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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|texte= VERIFYING ASTEROSEISMICALLY DETERMINED PARAMETERS OF KEPLER STARS USING HIPPARCOS PARALLAXES: SELF-CONSISTENT STELLAR PROPERTIES AND DISTANCES
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