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

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ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS

Identifieur interne : 007A68 ( Main/Exploration ); précédent : 007A67; suivant : 007A69

ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS

Auteurs : D. Huber [Australie] ; T. R. Bedding [Australie] ; D. Stello [Australie] ; B. Mosser [France] ; S. Mathur [États-Unis] ; T. Kallinger [Canada, Autriche] ; S. Hekker [Royaume-Uni] ; Y. P. Elsworth [Royaume-Uni] ; D. L. Buzasi [États-Unis] ; J. De Ridder [Belgique] ; R. L. Gilliland [États-Unis] ; H. Kjeldseni [Danemark] ; W. J. Chaplin [Royaume-Uni] ; R. A. Garcia [France] ; S. J. Hale [Royaume-Uni] ; H. L. Preston [États-Unis, Afrique du Sud] ; T. R. White [Australie] ; W. J. Borucki [États-Unis] ; J. Christensen-Dalsgaard [Danemark] ; B. D. Clarke [États-Unis] ; J. M. Jenkins [États-Unis] ; D. Koch [États-Unis]

Source :

RBID : Pascal:10-0518684

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English descriptors

Abstract

We have studied solar-like oscillations in ˜800 red giant stars using Kepler long-cadence photometry. The sample includes stars ranging in evolution from the lower part of the red giant branch to the helium main sequence. We investigate the relation between the large frequency separation (Δν) and the frequency of maximum power (νmax) and show that it is different for red giants than for main-sequence stars, which is consistent with evolutionary models and scaling relations. The distributions of νmax and Δν are in qualitative agreement with a simple stellar population model of the Kepler field, including the first evidence for a secondary clump population characterized by M ? 2 M◦. and νmax ≃ 40-110 μHz. We measured the small frequency separations δν02 and δν01 in over 400 stars and δν03 in over 40. We present C-D diagrams for I = 1, 2, and 3 and show that the frequency separation ratios δν02/Δν and δν01/Δν have opposite trends as a function of Δν. The data show a narrowing of the l = 1 ridge toward lower νmax, in agreement with models predicting more efficient mode trapping in stars with higher luminosity. We investigate the offset ∈ in the asymptotic relation and find a clear correlation with Δν, demonstrating that it is related to fundamental stellar parameters. Finally, we present the first amplitude-νmax relation for Kepler red giants. We observe a lack of low-amplitude stars for νmax ? 110 μHz and find that, for a given νmax between 40 and 110 μHz, stars with lower Δν (and consequently higher mass) tend to show lower amplitudes than stars with higher Δν.


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<title xml:lang="en" level="a">ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS</title>
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<name sortKey="Koch, D" sort="Koch, D" uniqKey="Koch D" first="D." last="Koch">D. Koch</name>
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<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="2010">2010</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>Correlations</term>
<term>Giant stars</term>
<term>Late type stars</term>
<term>Luminosity</term>
<term>Main sequence stars</term>
<term>Photometry</term>
<term>Physical parameter</term>
<term>Red giant stars</term>
<term>Red stars</term>
<term>Star models</term>
<term>Stellar evolution</term>
<term>Stellar population</term>
<term>Trend function</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr">
<term>Astéroséismologie</term>
<term>Géante rouge</term>
<term>Etoile rouge</term>
<term>Etoile géante</term>
<term>Photométrie</term>
<term>Evolution stellaire</term>
<term>Etoile séquence principale</term>
<term>Modèle stellaire</term>
<term>Population stellaire</term>
<term>Fonction tendance</term>
<term>Luminosité</term>
<term>Corrélation</term>
<term>Paramètre physique</term>
<term>Etoile type avancé</term>
</keywords>
</textClass>
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<front>
<div type="abstract" xml:lang="en">We have studied solar-like oscillations in ˜800 red giant stars using Kepler long-cadence photometry. The sample includes stars ranging in evolution from the lower part of the red giant branch to the helium main sequence. We investigate the relation between the large frequency separation (Δν) and the frequency of maximum power (ν
<sub>max</sub>
) and show that it is different for red giants than for main-sequence stars, which is consistent with evolutionary models and scaling relations. The distributions of ν
<sub>max</sub>
and Δν are in qualitative agreement with a simple stellar population model of the Kepler field, including the first evidence for a secondary clump population characterized by M ? 2 M
<sub>◦.</sub>
and ν
<sub>max</sub>
≃ 40-110 μHz. We measured the small frequency separations δν
<sub>02</sub>
and δν
<sub>01</sub>
in over 400 stars and δν
<sub>03</sub>
in over 40. We present C-D diagrams for I = 1, 2, and 3 and show that the frequency separation ratios δν
<sub>02</sub>
/Δν and δν
<sub>01</sub>
/Δν have opposite trends as a function of Δν. The data show a narrowing of the l = 1 ridge toward lower ν
<sub>max</sub>
, in agreement with models predicting more efficient mode trapping in stars with higher luminosity. We investigate the offset ∈ in the asymptotic relation and find a clear correlation with Δν, demonstrating that it is related to fundamental stellar parameters. Finally, we present the first amplitude-ν
<sub>max</sub>
relation for Kepler red giants. We observe a lack of low-amplitude stars for ν
<sub>max </sub>
? 110 μHz and find that, for a given ν
<sub>max</sub>
between 40 and 110 μHz, stars with lower Δν (and consequently higher mass) tend to show lower amplitudes than stars with higher Δν.</div>
</front>
</TEI>
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<list>
<country>
<li>Afrique du Sud</li>
<li>Australie</li>
<li>Autriche</li>
<li>Belgique</li>
<li>Canada</li>
<li>Danemark</li>
<li>France</li>
<li>Royaume-Uni</li>
<li>États-Unis</li>
</country>
<region>
<li>Angleterre</li>
<li>Midlands de l'Ouest</li>
<li>Nouvelle-Galles du Sud</li>
<li>Vienne (Autriche)</li>
<li>Île-de-France</li>
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<li>Birmingham</li>
<li>Gif-sur-Yvette</li>
<li>Meudon</li>
<li>Paris</li>
<li>Sydney</li>
<li>Vienne (Autriche)</li>
</settlement>
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<li>Université de Sydney</li>
</orgName>
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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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<region name="Vienne (Autriche)">
<name sortKey="Kallinger, T" sort="Kallinger, T" uniqKey="Kallinger T" first="T." last="Kallinger">T. Kallinger</name>
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