Solar-like oscillations from the depths of the red-giant star KIC 4351319 observed with Kepler
Identifieur interne : 004503 ( PascalFrancis/Curation ); précédent : 004502; suivant : 004504Solar-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.
Descripteurs français
- Pascal (Inist)
- Etoile rouge, Géante rouge, Etoile géante, Satellite Kepler, Rapport signal bruit, Fréquence oscillation, Température atmosphérique, Température effective, Gravité, Métallicité, Observation spectroscopique, Mode p, Modèle théorique, Combustion hydrogène, Age, Incertitude, Luminosité, Branche géante asymptotique, Evolution stellaire, Etoile type solaire.
English descriptors
- KwdEn :
- Age, Asymptotic giant branch, Atmospheric temperature, Effective temperature, Giant stars, Gravity, Hydrogen burning, Kepler satellite, Luminosity, Metallicity, Oscillation frequency, Red giant stars, Red stars, Signal-to-noise ratio, Solar type star, Spectroscopical observation, Stellar evolution, Theoretical model, Uncertainty, p mode.
Abstract
We present the results of the asteroseismic analysis of the red-giant star KIC 4351319 (TYC 3124-914-1), observed for 30d in short-cadence mode with the Kepler satellite. The analysis has allowed us to determine the large and small frequency separations, Δν0 = 24.6 ± 0.2 μHz and δν02 = 2.2 ± 0.3 μHz, respectively, and the frequency of maximum oscillation power, νmax = 386.5 ± 4.0 μHz. The high signal-to-noise ratio of the observations allowed us to identify 25 independent pulsation modes whose frequencies range approximately from 300 to 500 μHz. 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 ∼1.3M◦., a radius of ∼3.4R◦. 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.
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Leuven, Celestijnenlaan 200D</s1><s2>3001 Leuven</s2><s3>BEL</s3><sZ>8 aut.</sZ></inist:fA14><country>Belgique</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>9 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Science Park 904</s1><s2>1098 XH Amsterdam</s2><s3>NLD</s3><sZ>9 aut.</sZ></inist:fA14><country>Pays-Bas</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="04"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Kallinger, T" sort="Kallinger, T" uniqKey="Kallinger T" first="T." last="Kallinger">T. Kallinger</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, University of British Columbia</s1><s2>Vancouver</s2><s3>CAN</s3><sZ>11 aut.</sZ></inist:fA14><country>Canada</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Institute of Astronomy, University of Vienna</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>11 aut.</sZ></inist:fA14><country>Autriche</country></affiliation></author><author><name sortKey="Miglio, A" sort="Miglio, A" uniqKey="Miglio A" first="A." last="Miglio">A. 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Montalban</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>Institut d'Astrophysique et de Géofisique de l'Universitè de Liège, Allè du 6 Aout 17-B 4000 Liège</s1><s3>BEL</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Belgique</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="03"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>5 aut.</sZ><sZ>14 aut.</sZ></inist:fA14><country>France</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="04"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Uytterhoeven, K" sort="Uytterhoeven, K" uniqKey="Uytterhoeven K" first="K." last="Uytterhoeven">K. Uytterhoeven</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>16 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg im Breisgau</s1><s3>DEU</s3><sZ>16 aut.</sZ></inist:fA14><country>Allemagne</country></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="14"><s1>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field</s1><s2>CA 94035</s2><s3>USA</s3><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>États-Unis</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="05"><s1>Institutfor Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>7 aut.</sZ><sZ>18 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><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="15"><s1>SETI Institute/NASA Ames Research Center, Moffett Field</s1><s2>CA 94035</s2><s3>USA</s3><sZ>19 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Still, M" sort="Still, M" uniqKey="Still M" first="M." last="Still">M. Still</name><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field</s1><s2>CA 94035</s2><s3>USA</s3><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0372382</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0372382 INIST</idno><idno type="RBID">Pascal:11-0372382</idno><idno type="wicri:Area/PascalFrancis/Corpus">001A41</idno><idno type="wicri:Area/PascalFrancis/Curation">004503</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Solar-like oscillations from the depths of the red-giant star KIC 4351319 observed with Kepler</title><author><name sortKey="Di Mauro, M P" sort="Di Mauro, M P" uniqKey="Di Mauro M" first="M. P." last="Di Mauro">M. P. Di Mauro</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>INAF - IASF, Istituto di Astrofisíca Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100</s1><s2>00133 Roma</s2><s3>ITA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Cardini, D" sort="Cardini, D" uniqKey="Cardini D" first="D." last="Cardini">D. Cardini</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>INAF - IASF, Istituto di Astrofisíca Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100</s1><s2>00133 Roma</s2><s3>ITA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Catanzaro, G" sort="Catanzaro, G" uniqKey="Catanzaro G" first="G." last="Catanzaro">G. Catanzaro</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>INAF - Osservatorio Astrofisico di Catania, Via S. Sofia 78</s1><s2>95123 Catania</s2><s3>ITA</s3><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Ventura, R" sort="Ventura, R" uniqKey="Ventura R" first="R." last="Ventura">R. Ventura</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>INAF - Osservatorio Astrofisico di Catania, Via S. Sofia 78</s1><s2>95123 Catania</s2><s3>ITA</s3><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Barban, C" sort="Barban, C" uniqKey="Barban C" first="C." last="Barban">C. Barban</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>5 aut.</sZ><sZ>14 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="04"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>15 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="05"><s1>Institutfor Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>7 aut.</sZ><sZ>18 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><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="1"><inist:fA14 i1="06"><s1>Institut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D</s1><s2>3001 Leuven</s2><s3>BEL</s3><sZ>8 aut.</sZ></inist:fA14><country>Belgique</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>9 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Science Park 904</s1><s2>1098 XH Amsterdam</s2><s3>NLD</s3><sZ>9 aut.</sZ></inist:fA14><country>Pays-Bas</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="04"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Kallinger, T" sort="Kallinger, T" uniqKey="Kallinger T" first="T." last="Kallinger">T. Kallinger</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, University of British Columbia</s1><s2>Vancouver</s2><s3>CAN</s3><sZ>11 aut.</sZ></inist:fA14><country>Canada</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Institute of Astronomy, University of Vienna</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>11 aut.</sZ></inist:fA14><country>Autriche</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>9 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>Institut d'Astrophysique et de Géofisique de l'Universitè de Liège, Allè du 6 Aout 17-B 4000 Liège</s1><s3>BEL</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Belgique</country></affiliation></author><author><name sortKey="Montalban, J" sort="Montalban, J" uniqKey="Montalban J" first="J." last="Montalban">J. Montalban</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>Institut d'Astrophysique et de Géofisique de l'Universitè de Liège, Allè du 6 Aout 17-B 4000 Liège</s1><s3>BEL</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Belgique</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="03"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>5 aut.</sZ><sZ>14 aut.</sZ></inist:fA14><country>France</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="04"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Uytterhoeven, K" sort="Uytterhoeven, K" uniqKey="Uytterhoeven K" first="K." last="Uytterhoeven">K. Uytterhoeven</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>16 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg im Breisgau</s1><s3>DEU</s3><sZ>16 aut.</sZ></inist:fA14><country>Allemagne</country></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="14"><s1>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field</s1><s2>CA 94035</s2><s3>USA</s3><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>États-Unis</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="05"><s1>Institutfor Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>7 aut.</sZ><sZ>18 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><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="15"><s1>SETI Institute/NASA Ames Research Center, Moffett Field</s1><s2>CA 94035</s2><s3>USA</s3><sZ>19 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Still, M" sort="Still, M" uniqKey="Still M" first="M." last="Still">M. Still</name><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field</s1><s2>CA 94035</s2><s3>USA</s3><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Age</term><term>Asymptotic giant branch</term><term>Atmospheric temperature</term><term>Effective temperature</term><term>Giant stars</term><term>Gravity</term><term>Hydrogen burning</term><term>Kepler satellite</term><term>Luminosity</term><term>Metallicity</term><term>Oscillation frequency</term><term>Red giant stars</term><term>Red stars</term><term>Signal-to-noise ratio</term><term>Solar type star</term><term>Spectroscopical observation</term><term>Stellar evolution</term><term>Theoretical model</term><term>Uncertainty</term><term>p mode</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Etoile rouge</term><term>Géante rouge</term><term>Etoile géante</term><term>Satellite Kepler</term><term>Rapport signal bruit</term><term>Fréquence oscillation</term><term>Température atmosphérique</term><term>Température effective</term><term>Gravité</term><term>Métallicité</term><term>Observation spectroscopique</term><term>Mode p</term><term>Modèle théorique</term><term>Combustion hydrogène</term><term>Age</term><term>Incertitude</term><term>Luminosité</term><term>Branche géante asymptotique</term><term>Evolution stellaire</term><term>Etoile type solaire</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 30d in short-cadence mode with the Kepler satellite. The analysis has allowed us to determine the large and small frequency separations, Δν0 = 24.6 ± 0.2 μHz and δν02 = 2.2 ± 0.3 μHz, respectively, and the frequency of maximum oscillation power, νmax = 386.5 ± 4.0 μHz. The high signal-to-noise ratio of the observations allowed us to identify 25 independent pulsation modes whose frequencies range approximately from 300 to 500 μHz. 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 ∼1.3M◦., a radius of ∼3.4R◦. 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><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>415</s2></fA05><fA06><s2>4</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Solar-like oscillations from the depths of the red-giant star KIC 4351319 observed with Kepler</s1></fA08><fA11 i1="01" i2="1"><s1>DI MAURO (M. P.)</s1></fA11><fA11 i1="02" i2="1"><s1>CARDINI (D.)</s1></fA11><fA11 i1="03" i2="1"><s1>CATANZARO (G.)</s1></fA11><fA11 i1="04" i2="1"><s1>VENTURA (R.)</s1></fA11><fA11 i1="05" i2="1"><s1>BARBAN (C.)</s1></fA11><fA11 i1="06" i2="1"><s1>BEDDING (T. R.)</s1></fA11><fA11 i1="07" i2="1"><s1>CHRISTENSEN-DALSGAARD (J.)</s1></fA11><fA11 i1="08" i2="1"><s1>DE RIDDER (J.)</s1></fA11><fA11 i1="09" i2="1"><s1>HEKKER (S.)</s1></fA11><fA11 i1="10" i2="1"><s1>HUBER (D.)</s1></fA11><fA11 i1="11" i2="1"><s1>KALLINGER (T.)</s1></fA11><fA11 i1="12" i2="1"><s1>MIGLIO (A.)</s1></fA11><fA11 i1="13" i2="1"><s1>MONTALBAN (J.)</s1></fA11><fA11 i1="14" i2="1"><s1>MOSSER (B.)</s1></fA11><fA11 i1="15" i2="1"><s1>STELLO (D.)</s1></fA11><fA11 i1="16" i2="1"><s1>UYTTERHOEVEN (K.)</s1></fA11><fA11 i1="17" i2="1"><s1>KINEMUCHI (K.)</s1></fA11><fA11 i1="18" i2="1"><s1>KJELDSEN (H.)</s1></fA11><fA11 i1="19" i2="1"><s1>MULLALLY (F.)</s1></fA11><fA11 i1="20" i2="1"><s1>STILL (M.)</s1></fA11><fA14 i1="01"><s1>INAF - IASF, Istituto di Astrofisíca Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100</s1><s2>00133 Roma</s2><s3>ITA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></fA14><fA14 i1="02"><s1>INAF - Osservatorio Astrofisico di Catania, Via S. Sofia 78</s1><s2>95123 Catania</s2><s3>ITA</s3><sZ>3 aut.</sZ><sZ>4 aut.</sZ></fA14><fA14 i1="03"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>5 aut.</sZ><sZ>14 aut.</sZ></fA14><fA14 i1="04"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="05"><s1>Institutfor Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>7 aut.</sZ><sZ>18 aut.</sZ></fA14><fA14 i1="06"><s1>Institut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D</s1><s2>3001 Leuven</s2><s3>BEL</s3><sZ>8 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>9 aut.</sZ><sZ>12 aut.</sZ></fA14><fA14 i1="08"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Science Park 904</s1><s2>1098 XH Amsterdam</s2><s3>NLD</s3><sZ>9 aut.</sZ></fA14><fA14 i1="09"><s1>Department of Physics and Astronomy, University of British Columbia</s1><s2>Vancouver</s2><s3>CAN</s3><sZ>11 aut.</sZ></fA14><fA14 i1="10"><s1>Institute of Astronomy, University of Vienna</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>11 aut.</sZ></fA14><fA14 i1="11"><s1>Institut d'Astrophysique et de Géofisique de l'Universitè de Liège, Allè du 6 Aout 17-B 4000 Liège</s1><s3>BEL</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></fA14><fA14 i1="12"><s1>Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>16 aut.</sZ></fA14><fA14 i1="13"><s1>Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg im Breisgau</s1><s3>DEU</s3><sZ>16 aut.</sZ></fA14><fA14 i1="14"><s1>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field</s1><s2>CA 94035</s2><s3>USA</s3><sZ>17 aut.</sZ><sZ>20 aut.</sZ></fA14><fA14 i1="15"><s1>SETI Institute/NASA Ames Research Center, Moffett Field</s1><s2>CA 94035</s2><s3>USA</s3><sZ>19 aut.</sZ></fA14><fA20><s1>3783-3797</s1></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000508919600700</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0372382</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>USA</s0></fA66><fC01 i1="01" l="ENG"><s0>We present the results of the asteroseismic analysis of the red-giant star KIC 4351319 (TYC 3124-914-1), observed for 30d in short-cadence mode with the Kepler satellite. The analysis has allowed us to determine the large and small frequency separations, Δν0 = 24.6 ± 0.2 μHz and δν02 = 2.2 ± 0.3 μHz, respectively, and the frequency of maximum oscillation power, νmax = 386.5 ± 4.0 μHz. The high signal-to-noise ratio of the observations allowed us to identify 25 independent pulsation modes whose frequencies range approximately from 300 to 500 μHz. 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 ∼1.3M◦., a radius of ∼3.4R◦. 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.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Etoile rouge</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Red stars</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Géante rouge</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Red giant stars</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Etoile géante</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Giant stars</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Satellite Kepler</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Kepler satellite</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Satélite Kepler</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Rapport signal bruit</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Signal-to-noise ratio</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Fréquence oscillation</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Oscillation frequency</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Frecuencia oscilación</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Température atmosphérique</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Atmospheric temperature</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Température effective</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Effective temperature</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Gravité</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Gravity</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Métallicité</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Metallicity</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Metalicidad</s0><s5>35</s5></fC03><fC03 i1="11" i2="X" l="FRE"><s0>Observation spectroscopique</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="ENG"><s0>Spectroscopical observation</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="SPA"><s0>Observación espectroscópica</s0><s5>36</s5></fC03><fC03 i1="12" i2="X" l="FRE"><s0>Mode p</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="ENG"><s0>p mode</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="SPA"><s0>Modo p</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Modèle théorique</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Theoretical model</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Modelo teórico</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Combustion hydrogène</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Hydrogen burning</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Age</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Age</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Edad</s0><s5>40</s5></fC03><fC03 i1="16" i2="X" l="FRE"><s0>Incertitude</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="ENG"><s0>Uncertainty</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="SPA"><s0>Incertidumbre</s0><s5>41</s5></fC03><fC03 i1="17" i2="3" l="FRE"><s0>Luminosité</s0><s5>42</s5></fC03><fC03 i1="17" i2="3" l="ENG"><s0>Luminosity</s0><s5>42</s5></fC03><fC03 i1="18" i2="X" l="FRE"><s0>Branche géante asymptotique</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="ENG"><s0>Asymptotic giant branch</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="SPA"><s0>Rama gigante asintótica</s0><s5>43</s5></fC03><fC03 i1="19" i2="3" l="FRE"><s0>Evolution stellaire</s0><s5>44</s5></fC03><fC03 i1="19" i2="3" l="ENG"><s0>Stellar evolution</s0><s5>44</s5></fC03><fC03 i1="20" i2="X" l="FRE"><s0>Etoile type solaire</s0><s5>45</s5></fC03><fC03 i1="20" i2="X" l="ENG"><s0>Solar type star</s0><s5>45</s5></fC03><fC03 i1="20" i2="X" l="SPA"><s0>Estrella tipo solar</s0><s5>45</s5></fC03><fN21><s1>255</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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