AustralieFrV1, Main, Exploration, bibRecord, 006A82

GRANULATION IN RED GIANTS: OBSERVATIONS BY THE KEPLER MISSION AND THREE-DIMENSIONAL CONVECTION SIMULATIONS

Identifieur interne : 006A82 ( Main/Exploration ); précédent : 006A81; suivant : 006A83

GRANULATION IN RED GIANTS: OBSERVATIONS BY THE KEPLER MISSION AND THREE-DIMENSIONAL CONVECTION SIMULATIONS

Auteurs : S. Mathur [États-Unis] ; S. Hekker [Pays-Bas, Royaume-Uni] ; R. Trampedach [États-Unis] ; J. Ballot [France] ; T. Kallinger [Autriche, Belgique] ; D. Buzasi [États-Unis] ; R. A. Garcia [France] ; D. Huber [Australie] ; A. Jimenez [Espagne] ; B. Mosser [France] ; T. R. Bedding [Australie] ; Y. Elsworth [Royaume-Uni] ; C. Regulo [Espagne] ; D. Stello [Australie] ; W. J. Chaplin [Royaume-Uni] ; J. De Ridder [Belgique] ; S. J. Hale [Royaume-Uni] ; K. Kinemuchi [États-Unis] ; H. Kjeldsen [Danemark] ; F. Mullally [États-Unis] ; S. E. Thompson [États-Unis]

Source :

The Astrophysical journal [ 0004-637X ] ; 2011.

RBID : Pascal:11-0497923

Descripteurs français

Pascal (Inist)
- Géante rouge, Modèle 3 dimensions, Convection, Soleil, Plasma chaud, Granulation solaire, Astéroséismologie, Spectre puissance, Corrélation, Position, Masse stellaire, Paramètre physique, Gravité surface, Température effective, Analyse donnée, Etoile type avancé.

English descriptors

KwdEn :
- Astroseismology, Convection, Correlations, Data analysis, Effective temperature, Hot plasma, Late type stars, Physical parameter, Positions, Power spectra, Red giant stars, Solar granulation, Stellar mass, Sun, Surface gravity, Three dimensional model.

Abstract

The granulation pattern that we observe on the surface of the Sun is due to hot plasma rising to the photosphere where it cools down and descends back into the interior at the edges of granules. This is the visible manifestation of convection taking place in the outer part of the solar convection zone. Because red giants have deeper convection zones than the Sun, we cannot a priori assume that their granulation is a scaled version of solar granulation. Until now, neither observations nor one-dimensional analytical convection models could put constraints on granulation in red giants. With asteroseismology, this study can now be performed. We analyze ˜1000 red giants that have been observed by Kepler during 13 months. We fit the power spectra with Harvey-like profiles to retrieve the characteristics of the granulation (timescale τgran and power Pgran). We search for a correlation between these parameters and the global acoustic-mode parameter (the position of maximum power, vmax) as well as with stellar parameters (mass, radius, surface gravity (log g), and effective temperature (Teff)). We show that τeff v-0.89max and Pgran v-1.90max, which is consistent with the theoretical predictions. We find that the granulation timescales of stars that belong to the red clump have similar values while the timescales of stars in the red giant branch are spread in a wider range. Finally, we show that realistic three-dimensional simulations of the surface convection in stars, spanning the (Teff, log g) range of our sample of red giants, match the Kepler observations well in terms of trends.

Affiliations:

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Le document en format XML

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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">GRANULATION IN RED GIANTS: OBSERVATIONS BY THE KEPLER MISSION AND THREE-DIMENSIONAL CONVECTION SIMULATIONS</title>
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<author><name sortKey="Trampedach, R" sort="Trampedach, R" uniqKey="Trampedach R" first="R." last="Trampedach">R. Trampedach</name>
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</inist:fA14>
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<country>France</country>
<wicri:noRegion>92195 Meudon</wicri:noRegion>
<wicri:noRegion>Obs</wicri:noRegion>
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<country>Australie</country>
<placeName><settlement type="city">Sydney</settlement>
<region type="état">Nouvelle-Galles du Sud</region>
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<orgName type="university">Université de Sydney</orgName>
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<author><name sortKey="Elsworth, Y" sort="Elsworth, Y" uniqKey="Elsworth Y" first="Y." last="Elsworth">Y. Elsworth</name>
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<country>Royaume-Uni</country>
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<s2>38206, Tenerife</s2>
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<country>Espagne</country>
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</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Instituto de Astrofísica de Canarias, 38205, La Laguna</s1>
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<s3>ESP</s3>
<sZ>9 aut.</sZ>
<sZ>13 aut.</sZ>
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<country>Espagne</country>
<wicri:noRegion>Tenerife</wicri:noRegion>
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<author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name>
<affiliation wicri:level="4"><inist:fA14 i1="11"><s1>Sydney Institute for Astronomy, School of Physics, University of Sydney</s1>
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<sZ>8 aut.</sZ>
<sZ>11 aut.</sZ>
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<country>Australie</country>
<placeName><settlement type="city">Sydney</settlement>
<region type="état">Nouvelle-Galles du Sud</region>
</placeName>
<orgName type="university">Université de Sydney</orgName>
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</author>
<author><name sortKey="Chaplin, W J" sort="Chaplin, W J" uniqKey="Chaplin W" first="W. J." last="Chaplin">W. J. Chaplin</name>
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<country>Royaume-Uni</country>
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<orgName type="university">Université de Birmingham</orgName>
<placeName><settlement type="city">Birmingham</settlement>
<region type="country">Angleterre</region>
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</placeName>
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<author><name sortKey="De Ridder, J" sort="De Ridder, J" uniqKey="De Ridder J" first="J." last="De Ridder">J. De Ridder</name>
<affiliation wicri:level="3"><inist:fA14 i1="08"><s1>Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200D</s1>
<s2>3001 Leuven</s2>
<s3>BEL</s3>
<sZ>5 aut.</sZ>
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<country>Belgique</country>
<placeName><region type="province" nuts="2">Province du Brabant flamand</region>
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<author><name sortKey="Hale, S J" sort="Hale, S J" uniqKey="Hale S" first="S. J." last="Hale">S. J. Hale</name>
<affiliation wicri:level="4"><inist:fA14 i1="03"><s1>School of Physics and Astronomy, University of Birmingham, Edgbaston</s1>
<s2>Birmingham B15 2TT</s2>
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<sZ>2 aut.</sZ>
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<country>Royaume-Uni</country>
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<orgName type="university">Université de Birmingham</orgName>
<placeName><settlement type="city">Birmingham</settlement>
<region type="country">Angleterre</region>
<region type="région" nuts="1">Midlands de l'Ouest</region>
</placeName>
</affiliation>
</author>
<author><name sortKey="Kinemuchi, K" sort="Kinemuchi, K" uniqKey="Kinemuchi K" first="K." last="Kinemuchi">K. Kinemuchi</name>
<affiliation wicri:level="1"><inist:fA14 i1="15"><s1>Bay Area Environmental Research Inst./NASA Ames Research Center</s1>
<s2>Moffett Field, CA 94035</s2>
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<country>États-Unis</country>
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<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="16"><s1>Danish AsteroSeismology Centre, Department of Physics and Astronomy, University of Aarhus</s1>
<s2>8000 Aarhus</s2>
<s3>DNK</s3>
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<country>Danemark</country>
<wicri:noRegion>8000 Aarhus</wicri:noRegion>
</affiliation>
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<author><name sortKey="Mullally, F" sort="Mullally, F" uniqKey="Mullally F" first="F." last="Mullally">F. Mullally</name>
<affiliation wicri:level="1"><inist:fA14 i1="17"><s1>SETI Institute/NASA Ames Research Center</s1>
<s2>Moffett Field, CA 94035</s2>
<s3>USA</s3>
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<country>États-Unis</country>
<wicri:noRegion>SETI Institute/NASA Ames Research Center</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Thompson, S E" sort="Thompson, S E" uniqKey="Thompson S" first="S. E." last="Thompson">S. E. Thompson</name>
<affiliation wicri:level="1"><inist:fA14 i1="17"><s1>SETI Institute/NASA Ames Research Center</s1>
<s2>Moffett Field, CA 94035</s2>
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<sZ>20 aut.</sZ>
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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="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>Convection</term>
<term>Correlations</term>
<term>Data analysis</term>
<term>Effective temperature</term>
<term>Hot plasma</term>
<term>Late type stars</term>
<term>Physical parameter</term>
<term>Positions</term>
<term>Power spectra</term>
<term>Red giant stars</term>
<term>Solar granulation</term>
<term>Stellar mass</term>
<term>Sun</term>
<term>Surface gravity</term>
<term>Three dimensional model</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Géante rouge</term>
<term>Modèle 3 dimensions</term>
<term>Convection</term>
<term>Soleil</term>
<term>Plasma chaud</term>
<term>Granulation solaire</term>
<term>Astéroséismologie</term>
<term>Spectre puissance</term>
<term>Corrélation</term>
<term>Position</term>
<term>Masse stellaire</term>
<term>Paramètre physique</term>
<term>Gravité surface</term>
<term>Température effective</term>
<term>Analyse donnée</term>
<term>Etoile type avancé</term>
</keywords>
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<front><div type="abstract" xml:lang="en">The granulation pattern that we observe on the surface of the Sun is due to hot plasma rising to the photosphere where it cools down and descends back into the interior at the edges of granules. This is the visible manifestation of convection taking place in the outer part of the solar convection zone. Because red giants have deeper convection zones than the Sun, we cannot a priori assume that their granulation is a scaled version of solar granulation. Until now, neither observations nor one-dimensional analytical convection models could put constraints on granulation in red giants. With asteroseismology, this study can now be performed. We analyze ˜1000 red giants that have been observed by Kepler during 13 months. We fit the power spectra with Harvey-like profiles to retrieve the characteristics of the granulation (timescale τgran and power Pgran). We search for a correlation between these parameters and the global acoustic-mode parameter (the position of maximum power, vmax) as well as with stellar parameters (mass, radius, surface gravity (log g), and effective temperature (Teff)). We show that τeff  v-0.89max and Pgran  v-1.90max, which is consistent with the theoretical predictions. We find that the granulation timescales of stars that belong to the red clump have similar values while the timescales of stars in the red giant branch are spread in a wider range. Finally, we show that realistic three-dimensional simulations of the surface convection in stars, spanning the (Teff, log g) range of our sample of red giants, match the Kepler observations well in terms of trends.</div>
</front>
</TEI>
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<li>Autriche</li>
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<li>Pays-Bas</li>
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<orgName><li>Université Pierre-et-Marie-Curie</li>
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<country name="Pays-Bas"><region name="Hollande-Septentrionale"><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name>
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<country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name>
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<name sortKey="De Ridder, J" sort="De Ridder, J" uniqKey="De Ridder J" first="J." last="De Ridder">J. De Ridder</name>
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   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
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   |clé=     Pascal:11-0497923
   |texte=   GRANULATION IN RED GIANTS: OBSERVATIONS BY THE KEPLER MISSION AND THREE-DIMENSIONAL CONVECTION SIMULATIONS
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	Serveur d'exploration sur les relations entre la France et l'Australie
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Serveur d'exploration sur les relations entre la France et l'Australie

GRANULATION IN RED GIANTS: OBSERVATIONS BY THE KEPLER MISSION AND THREE-DIMENSIONAL CONVECTION SIMULATIONS

GRANULATION IN RED GIANTS: OBSERVATIONS BY THE KEPLER MISSION AND THREE-DIMENSIONAL CONVECTION SIMULATIONS

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