Serveur d'exploration sur les relations entre la France et l'Australie

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FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY

Identifieur interne : 005C59 ( Main/Exploration ); précédent : 005C58; suivant : 005C60

FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY

Auteurs : D. Huber [Australie, États-Unis] ; M. J. Ireland [Australie] ; T. R. Bedding [Australie] ; I. M. Brandao [Portugal] ; L. Piau [États-Unis] ; V. Maestro [Australie] ; T. R. White [Australie] ; H. Bruntt [Danemark] ; L. Casagrande [Australie] ; J. Molenda-Zakowicz [Pologne] ; V. Silva Aguirre [Danemark] ; S. G. Sousa [Portugal] ; T. Barclay [États-Unis] ; C. J. Burke [États-Unis] ; W. J. Chaplin [Danemark, Royaume-Uni] ; J. Christensen-Oalsgaard [Danemark] ; M. S. Cunha [Portugal] ; J. De Ridder [Belgique] ; C. D. Farrington [États-Unis] ; A. Frasca [Italie] ; R. A. Garcia [France] ; R. L. Gillil [États-Unis] ; P. J. Goldfinger [États-Unis] ; S. Hekker [Pays-Bas] ; S. D. Kawaler [États-Unis] ; H. Kjeldsen [Danemark] ; H. A. Mcalister [États-Unis] ; T. S. Metcalfe [États-Unis] ; A. Miglio [Royaume-Uni] ; M. J. P. F. G. Monteiro [Portugal] ; M. H. Pinsonneault [États-Unis] ; G. H. Schaefer [États-Unis] ; D. Stello [Australie] ; M. C. Stumpe [États-Unis] ; J. Sturmann [États-Unis] ; L. Sturmann [États-Unis] ; T. A. Ten Brummelaar [États-Unis] ; M. J. Thompson ; N. Turner [États-Unis] ; K. Uytterhoeven

Source :

RBID : Pascal:13-0018727

Descripteurs français

English descriptors

Abstract

We present results of a long-baseline interferometry campaign using the PAVO beam combiner at the CHARA Array to measure the angular sizes of five main-sequence stars, one subgiant and four red giant stars for which solar-like oscillations have been detected by either Kepler or CoRoT. By combining interferometric angular diameters, Hipparcos parallaxes, asteroseismic densities, bolometric fluxes, and high-resolution spectroscopy, we derive a full set of near-model-independent fundamental properties for the sample. We first use these properties to test asteroseismic scaling relations for the frequency of maximum power (vmax) and the large frequency separation (Δv). We find excellent agreement within the observational uncertainties, and empirically show that simple estimates of asteroseismic radii for main-sequence stars are accurate to ?4%. We furthermore find good agreement of our measured effective temperatures with spectroscopic and photometric estimates with mean deviations for stars between Teff = 4600-6200 K of -22 ± 32 K (with a scatter of 97 K) and -58 ± 31 K (with a scatter of 93 K), respectively. Finally, we present a first comparison with evolutionary models, and find differences between observed and theoretical properties for the metal-rich main-sequence star HD 173701. We conclude that the constraints presented in this study will have strong potential for testing stellar model physics, in particular when combined with detailed modeling of individual oscillation frequencies.


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<title xml:lang="en" level="a">FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY</title>
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<s1>School of Physics and Astronomy, University of Birmingham</s1>
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<s1>Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969</s1>
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<s1>Astronomical Institute "Anton Pannekoek," University of Amsterdam, Science Park 904</s1>
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<country>Pays-Bas</country>
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<s1>Department of Physics and Astronomy, Iowa State University</s1>
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<s1>Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969</s1>
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<s1>Space Science Institute</s1>
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<s1>School of Physics and Astronomy, University of Birmingham</s1>
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<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>
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<s1>Centro de Astrofõisica and Faculdade de Ciências, Universidade do Porto, Rua das Estrelas</s1>
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<s1>Department of Astronomy, Ohio State University</s1>
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<s1>Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969</s1>
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<s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1>
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<name sortKey="Stumpe, M C" sort="Stumpe, M C" uniqKey="Stumpe M" first="M. C." last="Stumpe">M. C. Stumpe</name>
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<s1>Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969</s1>
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<name sortKey="Sturmann, L" sort="Sturmann, L" uniqKey="Sturmann L" first="L." last="Sturmann">L. Sturmann</name>
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<s1>Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969</s1>
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<name sortKey="Ten Brummelaar, T A" sort="Ten Brummelaar, T A" uniqKey="Ten Brummelaar T" first="T. A." last="Ten Brummelaar">T. A. Ten Brummelaar</name>
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<s1>Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969</s1>
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<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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<author>
<name sortKey="Turner, N" sort="Turner, N" uniqKey="Turner N" first="N." last="Turner">N. Turner</name>
<affiliation wicri:level="1">
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<s1>Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969</s1>
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<author>
<name sortKey="Uytterhoeven, K" sort="Uytterhoeven, K" uniqKey="Uytterhoeven K" first="K." last="Uytterhoeven">K. Uytterhoeven</name>
</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>Angular diameter</term>
<term>Angular dimension</term>
<term>Astroseismology</term>
<term>Effective temperature</term>
<term>Flux density</term>
<term>Giant stars</term>
<term>Interferometry</term>
<term>Late type stars</term>
<term>Main sequence stars</term>
<term>Modelling</term>
<term>Oscillation frequency</term>
<term>Red giant stars</term>
<term>Red stars</term>
<term>Spectroscopy</term>
<term>Star models</term>
<term>Stellar pulsations</term>
<term>Subgiant star</term>
<term>Uncertainty</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr">
<term>Astéroséismologie</term>
<term>Interférométrie</term>
<term>Dimension angulaire</term>
<term>Etoile séquence principale</term>
<term>Sous géante</term>
<term>Etoile rouge</term>
<term>Géante rouge</term>
<term>Etoile géante</term>
<term>Diamètre angulaire</term>
<term>Densité flux</term>
<term>Spectrométrie</term>
<term>Modèle stellaire</term>
<term>Incertitude</term>
<term>Température effective</term>
<term>Modélisation</term>
<term>Fréquence oscillation</term>
<term>Etoile type avancé</term>
<term>Pulsation stellaire</term>
</keywords>
<keywords scheme="Wicri" type="topic" xml:lang="fr">
<term>Spectrométrie</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front>
<div type="abstract" xml:lang="en">We present results of a long-baseline interferometry campaign using the PAVO beam combiner at the CHARA Array to measure the angular sizes of five main-sequence stars, one subgiant and four red giant stars for which solar-like oscillations have been detected by either Kepler or CoRoT. By combining interferometric angular diameters, Hipparcos parallaxes, asteroseismic densities, bolometric fluxes, and high-resolution spectroscopy, we derive a full set of near-model-independent fundamental properties for the sample. We first use these properties to test asteroseismic scaling relations for the frequency of maximum power (v
<sub>max</sub>
) and the large frequency separation (Δv). We find excellent agreement within the observational uncertainties, and empirically show that simple estimates of asteroseismic radii for main-sequence stars are accurate to ?4%. We furthermore find good agreement of our measured effective temperatures with spectroscopic and photometric estimates with mean deviations for stars between T
<sub>eff</sub>
= 4600-6200 K of -22 ± 32 K (with a scatter of 97 K) and -58 ± 31 K (with a scatter of 93 K), respectively. Finally, we present a first comparison with evolutionary models, and find differences between observed and theoretical properties for the metal-rich main-sequence star HD 173701. We conclude that the constraints presented in this study will have strong potential for testing stellar model physics, in particular when combined with detailed modeling of individual oscillation frequencies.</div>
</front>
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<li>Australie</li>
<li>Belgique</li>
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<li>Pologne</li>
<li>Portugal</li>
<li>Royaume-Uni</li>
<li>États-Unis</li>
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<li>Angleterre</li>
<li>Hollande-Septentrionale</li>
<li>Iowa</li>
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<li>Province du Brabant flamand</li>
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<li>Université d'État de l'Iowa</li>
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<li>Université de Sydney</li>
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<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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<country name="Australie">
<region name="Nouvelle-Galles du Sud">
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