AustralieFrV1, Istex, Curation, bibRecord, 000149

Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler

Identifieur interne : 000149 ( Istex/Curation ); précédent : 000148; suivant : 000150

Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler

Auteurs : M. P. Di Mauro [Italie] ; D. Cardini [Italie] ; G. Catanzaro [Italie] ; R. Ventura [Italie] ; C. Barban [France] ; T. R. Bedding [Australie] ; J. Christensen-Dalsgaard [Danemark] ; J. De Ridder [Belgique] ; S. Hekker [Royaume-Uni, Pays-Bas] ; D. Huber [Australie] ; T. Kallinger [Canada, Autriche] ; A. Miglio [Royaume-Uni, Belgique] ; J. Montalban [Belgique] ; B. Mosser [France] ; D. Stello [Australie] ; K. Uytterhoeven [France, Allemagne] ; K. Kinemuchi [États-Unis] ; H. Kjeldsen [Danemark] ; F. Mullally [États-Unis] ; M. Still [États-Unis]

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-08-21.

RBID : ISTEX:07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C

English descriptors

Abstract

We present the results of the asteroseismic analysis of the red‐giant star KIC 4351319 (TYC 3124‐914‐1), observed for 30 d in short‐cadence mode with the Kepler satellite. The analysis has allowed us to determine the large and small frequency separations, Hz and Hz, respectively, and the frequency of maximum oscillation power, Hz. The high signal‐to‐noise ratio of the observations allowed us to identify 25 independent pulsation modes whose frequencies range approximately from 300 to Hz. The observed oscillation frequencies together with the accurate determination of the atmospheric parameters (effective temperature, gravity and metallicity), provided by additional ground‐based spectroscopic observations, enabled us to theoretically interpret the observed oscillation spectrum. KIC 4351319 appears to oscillate with a well‐defined solar‐type p‐mode pattern due to radial acoustic modes and non‐radial nearly pure p modes. In addition, several non‐radial mixed modes have been identified. Theoretical models well reproduce the observed oscillation frequencies and indicate that this star, located at the base of the ascending red‐giant branch, is in the hydrogen‐shell‐burning phase, with a mass of ∼1.3 M⊙, a radius of and an age of ∼5.6 Gyr. The main parameters of this star have been determined with an unprecedented level of precision for a red‐giant star, with uncertainties of 2 per cent for mass, 7 per cent for age, 1 per cent for radius and 4 per cent for luminosity.

Url:

https://api.istex.fr/document/07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C/fulltext/pdf

DOI: 10.1111/j.1365-2966.2011.18996.x

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Le document en format XML

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<sourceDesc><biblStruct><analytic><title level="a" type="main">Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with <hi rend="italic">Kepler</hi>
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<author><name sortKey="Christensen Alsgaard, J" sort="Christensen Alsgaard, J" uniqKey="Christensen Alsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name>
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<country xml:lang="fr">Belgique</country>
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</affiliation>
</author>
<author><name sortKey="Montalban, J" sort="Montalban, J" uniqKey="Montalban J" first="J." last="Montalban">J. Montalban</name>
<affiliation wicri:level="1"><mods:affiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</mods:affiliation>
<country xml:lang="fr">Belgique</country>
<wicri:regionArea>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name>
<affiliation wicri:level="1"><mods:affiliation>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France</mods:affiliation>
<country xml:lang="fr">France</country>
<wicri:regionArea>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name>
<affiliation wicri:level="1"><mods:affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</mods:affiliation>
<country xml:lang="fr">Australie</country>
<wicri:regionArea>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Uytterhoeven, K" sort="Uytterhoeven, K" uniqKey="Uytterhoeven K" first="K." last="Uytterhoeven">K. Uytterhoeven</name>
<affiliation wicri:level="1"><mods:affiliation>Laboratoire AIM, CEA/DSM‐CNRS‐Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay, 91191 Gif‐sur‐Yvette, France</mods:affiliation>
<country xml:lang="fr">France</country>
<wicri:regionArea>Laboratoire AIM, CEA/DSM‐CNRS‐Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay, 91191 Gif‐sur‐Yvette</wicri:regionArea>
</affiliation>
<affiliation wicri:level="1"><mods:affiliation>Kiepenheuer‐Institut für Sonnenphysik, Schöneckstraße 6, 79104 Freiburg im Breisgau, Germany</mods:affiliation>
<country xml:lang="fr">Allemagne</country>
<wicri:regionArea>Kiepenheuer‐Institut für Sonnenphysik, Schöneckstraße 6, 79104 Freiburg im Breisgau</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Kinemuchi, K" sort="Kinemuchi, K" uniqKey="Kinemuchi K" first="K." last="Kinemuchi">K. Kinemuchi</name>
<affiliation wicri:level="1"><mods:affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation>
<country xml:lang="fr">États-Unis</country>
<wicri:regionArea>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name>
<affiliation wicri:level="1"><mods:affiliation>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark</mods:affiliation>
<country xml:lang="fr">Danemark</country>
<wicri:regionArea>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Mullally, F" sort="Mullally, F" uniqKey="Mullally F" first="F." last="Mullally">F. Mullally</name>
<affiliation wicri:level="1"><mods:affiliation>SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation>
<country xml:lang="fr">États-Unis</country>
<wicri:regionArea>SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Still, M" sort="Still, M" uniqKey="Still M" first="M." last="Still">M. Still</name>
<affiliation wicri:level="1"><mods:affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation>
<country xml:lang="fr">États-Unis</country>
<wicri:regionArea>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035</wicri:regionArea>
</affiliation>
</author>
</analytic>
<monogr></monogr>
<series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title>
<idno type="ISSN">0035-8711</idno>
<idno type="eISSN">1365-2966</idno>
<imprint><biblScope unit="vol">415</biblScope>
<biblScope unit="issue">4</biblScope>
<biblScope unit="page" from="3783">3783</biblScope>
<biblScope unit="page" to="3797">3797</biblScope>
<biblScope unit="page-count">15</biblScope>
<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<date type="published" when="2011-08-21">2011-08-21</date>
</imprint>
<idno type="ISSN">0035-8711</idno>
</series>
</biblStruct>
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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Abundance pattern</term>
<term>Acoustic</term>
<term>Acoustic modes</term>
<term>Acoustic radius</term>
<term>Acoustic waves</term>
<term>Acoustical frequency</term>
<term>Additional effects</term>
<term>Adiabatic</term>
<term>Adiabatic frequencies</term>
<term>Allende prieto</term>
<term>Astron</term>
<term>Atlas9 code</term>
<term>Atmospheric parameters</term>
<term>Background model</term>
<term>Bedding</term>
<term>Bedding kjeldsen</term>
<term>Binned power spectrum</term>
<term>Blue triangles</term>
<term>Bottom panel</term>
<term>Buoyancy frequency</term>
<term>Cambridge univ</term>
<term>Central frequency</term>
<term>Convective</term>
<term>Convective envelope</term>
<term>Direct modelling</term>
<term>Echelle</term>
<term>Echelle diagram</term>
<term>Echelle diagrams</term>
<term>Effective temperature</term>
<term>Effective temperature ranges</term>
<term>Envelope autocorrelation function analysis</term>
<term>Evolutionary phase</term>
<term>Evolutionary state</term>
<term>Free parameters</term>
<term>Frequency</term>
<term>Frequency range</term>
<term>Frequency resolution</term>
<term>Global asteroseismic parameters</term>
<term>Good agreement</term>
<term>Gravity character</term>
<term>Gravity waves</term>
<term>Grey dots</term>
<term>Harmonic</term>
<term>Harmonic degree</term>
<term>Hekker</term>
<term>High frequencies</term>
<term>High inertia</term>
<term>Huber</term>
<term>Hydrogen abundance</term>
<term>Independent averages</term>
<term>Individual frequencies</term>
<term>Inertia</term>
<term>Initial hydrogen abundance</term>
<term>Integration time</term>
<term>Ionization</term>
<term>Iron abundance</term>
<term>Kallinger</term>
<term>Kepler</term>
<term>Kepler satellite</term>
<term>Kjeldsen</term>
<term>Kjeldsen bedding</term>
<term>Lamb frequencies</term>
<term>Large frequency separation</term>
<term>Large separation</term>
<term>Light curve</term>
<term>Lled symbols</term>
<term>Lower frequencies</term>
<term>Lower panel</term>
<term>Luminosity</term>
<term>Main parameters</term>
<term>Mauro</term>
<term>Maximum amplitude</term>
<term>Mcdonald observatory</term>
<term>Miglio</term>
<term>Mnras</term>
<term>Mode</term>
<term>Mode degree</term>
<term>Mode lifetime</term>
<term>Mode width</term>
<term>Moffett field</term>
<term>Monthly notices</term>
<term>Mosser</term>
<term>Mosser appourchaux</term>
<term>Nancial support</term>
<term>Open symbols</term>
<term>Oscillation</term>
<term>Oscillation frequencies</term>
<term>Oscillation modes</term>
<term>Oscillation properties</term>
<term>Oscillation spectra</term>
<term>Oscillation spectrum</term>
<term>Oscillatory signal</term>
<term>Other parameters</term>
<term>Overshooting</term>
<term>Parameter</term>
<term>Period spacings</term>
<term>Photon noise</term>
<term>Power density spectrum</term>
<term>Power spectrum</term>
<term>Present analysis</term>
<term>Pressure scaleheight</term>
<term>Prevalent character</term>
<term>Propagation diagram</term>
<term>Publications division</term>
<term>Radial</term>
<term>Radial mode</term>
<term>Radial modes</term>
<term>Radial order</term>
<term>Regular spacing</term>
<term>Relative surface amplitude</term>
<term>Results show</term>
<term>Rotational</term>
<term>Rotational splitting</term>
<term>Rotational splittings</term>
<term>Same frequency</term>
<term>Second ionization</term>
<term>Sharp features</term>
<term>Sharp variation</term>
<term>Similar frequencies</term>
<term>Small frequency separation</term>
<term>Small frequency separations</term>
<term>Small separation</term>
<term>Small separations</term>
<term>Solid lines</term>
<term>Spectral window</term>
<term>Spectroscopic</term>
<term>Spectroscopic constraints</term>
<term>Spectroscopic observations</term>
<term>Spectrum</term>
<term>Standard deviation</term>
<term>Stellar</term>
<term>Stellar activity</term>
<term>Stellar background</term>
<term>Stellar spectrum</term>
<term>Stellar structure</term>
<term>Straight line</term>
<term>Strong character</term>
<term>Surface gravity</term>
<term>Theoretical frequencies</term>
<term>Theoretical models</term>
<term>Thermodynamic properties</term>
<term>Tted</term>
<term>Tting</term>
<term>Turbulent diffusion</term>
<term>Unprecedented level</term>
<term>Upper panel</term>
<term>Vertical line</term>
<term>White noise</term>
<term>Window function</term>
</keywords>
<keywords scheme="Teeft" xml:lang="en"><term>Abundance pattern</term>
<term>Acoustic</term>
<term>Acoustic modes</term>
<term>Acoustic radius</term>
<term>Acoustic waves</term>
<term>Acoustical frequency</term>
<term>Additional effects</term>
<term>Adiabatic</term>
<term>Adiabatic frequencies</term>
<term>Allende prieto</term>
<term>Astron</term>
<term>Atlas9 code</term>
<term>Atmospheric parameters</term>
<term>Background model</term>
<term>Bedding</term>
<term>Bedding kjeldsen</term>
<term>Binned power spectrum</term>
<term>Blue triangles</term>
<term>Bottom panel</term>
<term>Buoyancy frequency</term>
<term>Cambridge univ</term>
<term>Central frequency</term>
<term>Convective</term>
<term>Convective envelope</term>
<term>Direct modelling</term>
<term>Echelle</term>
<term>Echelle diagram</term>
<term>Echelle diagrams</term>
<term>Effective temperature</term>
<term>Effective temperature ranges</term>
<term>Envelope autocorrelation function analysis</term>
<term>Evolutionary phase</term>
<term>Evolutionary state</term>
<term>Free parameters</term>
<term>Frequency</term>
<term>Frequency range</term>
<term>Frequency resolution</term>
<term>Global asteroseismic parameters</term>
<term>Good agreement</term>
<term>Gravity character</term>
<term>Gravity waves</term>
<term>Grey dots</term>
<term>Harmonic</term>
<term>Harmonic degree</term>
<term>Hekker</term>
<term>High frequencies</term>
<term>High inertia</term>
<term>Huber</term>
<term>Hydrogen abundance</term>
<term>Independent averages</term>
<term>Individual frequencies</term>
<term>Inertia</term>
<term>Initial hydrogen abundance</term>
<term>Integration time</term>
<term>Ionization</term>
<term>Iron abundance</term>
<term>Kallinger</term>
<term>Kepler</term>
<term>Kepler satellite</term>
<term>Kjeldsen</term>
<term>Kjeldsen bedding</term>
<term>Lamb frequencies</term>
<term>Large frequency separation</term>
<term>Large separation</term>
<term>Light curve</term>
<term>Lled symbols</term>
<term>Lower frequencies</term>
<term>Lower panel</term>
<term>Luminosity</term>
<term>Main parameters</term>
<term>Mauro</term>
<term>Maximum amplitude</term>
<term>Mcdonald observatory</term>
<term>Miglio</term>
<term>Mnras</term>
<term>Mode</term>
<term>Mode degree</term>
<term>Mode lifetime</term>
<term>Mode width</term>
<term>Moffett field</term>
<term>Monthly notices</term>
<term>Mosser</term>
<term>Mosser appourchaux</term>
<term>Nancial support</term>
<term>Open symbols</term>
<term>Oscillation</term>
<term>Oscillation frequencies</term>
<term>Oscillation modes</term>
<term>Oscillation properties</term>
<term>Oscillation spectra</term>
<term>Oscillation spectrum</term>
<term>Oscillatory signal</term>
<term>Other parameters</term>
<term>Overshooting</term>
<term>Parameter</term>
<term>Period spacings</term>
<term>Photon noise</term>
<term>Power density spectrum</term>
<term>Power spectrum</term>
<term>Present analysis</term>
<term>Pressure scaleheight</term>
<term>Prevalent character</term>
<term>Propagation diagram</term>
<term>Publications division</term>
<term>Radial</term>
<term>Radial mode</term>
<term>Radial modes</term>
<term>Radial order</term>
<term>Regular spacing</term>
<term>Relative surface amplitude</term>
<term>Results show</term>
<term>Rotational</term>
<term>Rotational splitting</term>
<term>Rotational splittings</term>
<term>Same frequency</term>
<term>Second ionization</term>
<term>Sharp features</term>
<term>Sharp variation</term>
<term>Similar frequencies</term>
<term>Small frequency separation</term>
<term>Small frequency separations</term>
<term>Small separation</term>
<term>Small separations</term>
<term>Solid lines</term>
<term>Spectral window</term>
<term>Spectroscopic</term>
<term>Spectroscopic constraints</term>
<term>Spectroscopic observations</term>
<term>Spectrum</term>
<term>Standard deviation</term>
<term>Stellar</term>
<term>Stellar activity</term>
<term>Stellar background</term>
<term>Stellar spectrum</term>
<term>Stellar structure</term>
<term>Straight line</term>
<term>Strong character</term>
<term>Surface gravity</term>
<term>Theoretical frequencies</term>
<term>Theoretical models</term>
<term>Thermodynamic properties</term>
<term>Tted</term>
<term>Tting</term>
<term>Turbulent diffusion</term>
<term>Unprecedented level</term>
<term>Upper panel</term>
<term>Vertical line</term>
<term>White noise</term>
<term>Window function</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">We present the results of the asteroseismic analysis of the red‐giant star KIC 4351319 (TYC 3124‐914‐1), observed for 30 d in short‐cadence mode with the Kepler satellite. The analysis has allowed us to determine the large and small frequency separations, Hz and Hz, respectively, and the frequency of maximum oscillation power, Hz. The high signal‐to‐noise ratio of the observations allowed us to identify 25 independent pulsation modes whose frequencies range approximately from 300 to Hz. The observed oscillation frequencies together with the accurate determination of the atmospheric parameters (effective temperature, gravity and metallicity), provided by additional ground‐based spectroscopic observations, enabled us to theoretically interpret the observed oscillation spectrum. KIC 4351319 appears to oscillate with a well‐defined solar‐type p‐mode pattern due to radial acoustic modes and non‐radial nearly pure p modes. In addition, several non‐radial mixed modes have been identified. Theoretical models well reproduce the observed oscillation frequencies and indicate that this star, located at the base of the ascending red‐giant branch, is in the hydrogen‐shell‐burning phase, with a mass of ∼1.3 M⊙, a radius of and an age of ∼5.6 Gyr. The main parameters of this star have been determined with an unprecedented level of precision for a red‐giant star, with uncertainties of 2 per cent for mass, 7 per cent for age, 1 per cent for radius and 4 per cent for luminosity.</div>
</front>
</TEI>
</record>

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Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler

Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler

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