Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler
Identifieur interne : 000149 ( Istex/Corpus ); précédent : 000148; suivant : 000150Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler
Auteurs : M. P. Di Mauro ; D. Cardini ; G. Catanzaro ; R. Ventura ; C. Barban ; T. R. Bedding ; J. Christensen-Dalsgaard ; J. De Ridder ; S. Hekker ; D. Huber ; T. Kallinger ; A. Miglio ; J. Montalban ; B. Mosser ; D. Stello ; K. Uytterhoeven ; K. Kinemuchi ; H. Kjeldsen ; F. Mullally ; M. StillSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-08-21.
English descriptors
- KwdEn :
- Abundance pattern, Acoustic, Acoustic modes, Acoustic radius, Acoustic waves, Acoustical frequency, Additional effects, Adiabatic, Adiabatic frequencies, Allende prieto, Astron, Atlas9 code, Atmospheric parameters, Background model, Bedding, Bedding kjeldsen, Binned power spectrum, Blue triangles, Bottom panel, Buoyancy frequency, Cambridge univ, Central frequency, Convective, Convective envelope, Direct modelling, Echelle, Echelle diagram, Echelle diagrams, Effective temperature, Effective temperature ranges, Envelope autocorrelation function analysis, Evolutionary phase, Evolutionary state, Free parameters, Frequency, Frequency range, Frequency resolution, Global asteroseismic parameters, Good agreement, Gravity character, Gravity waves, Grey dots, Harmonic, Harmonic degree, Hekker, High frequencies, High inertia, Huber, Hydrogen abundance, Independent averages, Individual frequencies, Inertia, Initial hydrogen abundance, Integration time, Ionization, Iron abundance, Kallinger, Kepler, Kepler satellite, Kjeldsen, Kjeldsen bedding, Lamb frequencies, Large frequency separation, Large separation, Light curve, Lled symbols, Lower frequencies, Lower panel, Luminosity, Main parameters, Mauro, Maximum amplitude, Mcdonald observatory, Miglio, Mnras, Mode, Mode degree, Mode lifetime, Mode width, Moffett field, Monthly notices, Mosser, Mosser appourchaux, Nancial support, Open symbols, Oscillation, Oscillation frequencies, Oscillation modes, Oscillation properties, Oscillation spectra, Oscillation spectrum, Oscillatory signal, Other parameters, Overshooting, Parameter, Period spacings, Photon noise, Power density spectrum, Power spectrum, Present analysis, Pressure scaleheight, Prevalent character, Propagation diagram, Publications division, Radial, Radial mode, Radial modes, Radial order, Regular spacing, Relative surface amplitude, Results show, Rotational, Rotational splitting, Rotational splittings, Same frequency, Second ionization, Sharp features, Sharp variation, Similar frequencies, Small frequency separation, Small frequency separations, Small separation, Small separations, Solid lines, Spectral window, Spectroscopic, Spectroscopic constraints, Spectroscopic observations, Spectrum, Standard deviation, Stellar, Stellar activity, Stellar background, Stellar spectrum, Stellar structure, Straight line, Strong character, Surface gravity, Theoretical frequencies, Theoretical models, Thermodynamic properties, Tted, Tting, Turbulent diffusion, Unprecedented level, Upper panel, Vertical line, White noise, Window function.
- Teeft :
- Abundance pattern, Acoustic, Acoustic modes, Acoustic radius, Acoustic waves, Acoustical frequency, Additional effects, Adiabatic, Adiabatic frequencies, Allende prieto, Astron, Atlas9 code, Atmospheric parameters, Background model, Bedding, Bedding kjeldsen, Binned power spectrum, Blue triangles, Bottom panel, Buoyancy frequency, Cambridge univ, Central frequency, Convective, Convective envelope, Direct modelling, Echelle, Echelle diagram, Echelle diagrams, Effective temperature, Effective temperature ranges, Envelope autocorrelation function analysis, Evolutionary phase, Evolutionary state, Free parameters, Frequency, Frequency range, Frequency resolution, Global asteroseismic parameters, Good agreement, Gravity character, Gravity waves, Grey dots, Harmonic, Harmonic degree, Hekker, High frequencies, High inertia, Huber, Hydrogen abundance, Independent averages, Individual frequencies, Inertia, Initial hydrogen abundance, Integration time, Ionization, Iron abundance, Kallinger, Kepler, Kepler satellite, Kjeldsen, Kjeldsen bedding, Lamb frequencies, Large frequency separation, Large separation, Light curve, Lled symbols, Lower frequencies, Lower panel, Luminosity, Main parameters, Mauro, Maximum amplitude, Mcdonald observatory, Miglio, Mnras, Mode, Mode degree, Mode lifetime, Mode width, Moffett field, Monthly notices, Mosser, Mosser appourchaux, Nancial support, Open symbols, Oscillation, Oscillation frequencies, Oscillation modes, Oscillation properties, Oscillation spectra, Oscillation spectrum, Oscillatory signal, Other parameters, Overshooting, Parameter, Period spacings, Photon noise, Power density spectrum, Power spectrum, Present analysis, Pressure scaleheight, Prevalent character, Propagation diagram, Publications division, Radial, Radial mode, Radial modes, Radial order, Regular spacing, Relative surface amplitude, Results show, Rotational, Rotational splitting, Rotational splittings, Same frequency, Second ionization, Sharp features, Sharp variation, Similar frequencies, Small frequency separation, Small frequency separations, Small separation, Small separations, Solid lines, Spectral window, Spectroscopic, Spectroscopic constraints, Spectroscopic observations, Spectrum, Standard deviation, Stellar, Stellar activity, Stellar background, Stellar spectrum, Stellar structure, Straight line, Strong character, Surface gravity, Theoretical frequencies, Theoretical models, Thermodynamic properties, Tted, Tting, Turbulent diffusion, Unprecedented level, Upper panel, Vertical line, White noise, Window function.
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:
DOI: 10.1111/j.1365-2966.2011.18996.x
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<record><TEI wicri:istexFullTextTei="biblStruct"><teiHeader><fileDesc><titleStmt><title xml:lang="en">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><mods:affiliation>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: mariapia.dimauro@iasf‐roma.inaf.it</mods:affiliation></affiliation></author><author><name sortKey="Cardini, D" sort="Cardini, D" uniqKey="Cardini D" first="D." last="Cardini">D. Cardini</name><affiliation><mods:affiliation>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy</mods:affiliation></affiliation></author><author><name sortKey="Catanzaro, G" sort="Catanzaro, G" uniqKey="Catanzaro G" first="G." last="Catanzaro">G. Catanzaro</name><affiliation><mods:affiliation>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</mods:affiliation></affiliation></author><author><name sortKey="Ventura, R" sort="Ventura, R" uniqKey="Ventura R" first="R." last="Ventura">R. Ventura</name><affiliation><mods:affiliation>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</mods:affiliation></affiliation></author><author><name sortKey="Barban, C" sort="Barban, C" uniqKey="Barban C" first="C." last="Barban">C. Barban</name><affiliation><mods:affiliation>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France</mods:affiliation></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><mods:affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation></author><author><name sortKey="Christensen Alsgaard, J" sort="Christensen Alsgaard, J" uniqKey="Christensen Alsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name><affiliation><mods:affiliation>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark</mods:affiliation></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><mods:affiliation>Institut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium</mods:affiliation></affiliation></author><author><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name><affiliation><mods:affiliation>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</mods:affiliation></affiliation><affiliation><mods:affiliation>Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands</mods:affiliation></affiliation></author><author><name sortKey="Huber, D" sort="Huber, D" uniqKey="Huber D" first="D." last="Huber">D. Huber</name><affiliation><mods:affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation></author><author><name sortKey="Kallinger, T" sort="Kallinger, T" uniqKey="Kallinger T" first="T." last="Kallinger">T. Kallinger</name><affiliation><mods:affiliation>Department of Physics and Astronomy, University of British Columbia, Vancouver, Canada</mods:affiliation></affiliation><affiliation><mods:affiliation>Institute of Astronomy, University of Vienna, 1180 Vienna, Austria</mods:affiliation></affiliation></author><author><name sortKey="Miglio, A" sort="Miglio, A" uniqKey="Miglio A" first="A." last="Miglio">A. Miglio</name><affiliation><mods:affiliation>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</mods:affiliation></affiliation><affiliation><mods:affiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</mods:affiliation></affiliation></author><author><name sortKey="Montalban, J" sort="Montalban, J" uniqKey="Montalban J" first="J." last="Montalban">J. Montalban</name><affiliation><mods:affiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</mods:affiliation></affiliation></author><author><name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name><affiliation><mods:affiliation>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France</mods:affiliation></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation><mods:affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation></author><author><name sortKey="Uytterhoeven, K" sort="Uytterhoeven, K" uniqKey="Uytterhoeven K" first="K." last="Uytterhoeven">K. Uytterhoeven</name><affiliation><mods:affiliation>Laboratoire AIM, CEA/DSM‐CNRS‐Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay, 91191 Gif‐sur‐Yvette, France</mods:affiliation></affiliation><affiliation><mods:affiliation>Kiepenheuer‐Institut für Sonnenphysik, Schöneckstraße 6, 79104 Freiburg im Breisgau, Germany</mods:affiliation></affiliation></author><author><name sortKey="Kinemuchi, K" sort="Kinemuchi, K" uniqKey="Kinemuchi K" first="K." last="Kinemuchi">K. Kinemuchi</name><affiliation><mods:affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation><mods:affiliation>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark</mods:affiliation></affiliation></author><author><name sortKey="Mullally, F" sort="Mullally, F" uniqKey="Mullally F" first="F." last="Mullally">F. Mullally</name><affiliation><mods:affiliation>SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation></affiliation></author><author><name sortKey="Still, M" sort="Still, M" uniqKey="Still M" first="M." last="Still">M. Still</name><affiliation><mods:affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C</idno><date when="2011" year="2011">2011</date><idno type="doi">10.1111/j.1365-2966.2011.18996.x</idno><idno type="url">https://api.istex.fr/document/07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">000149</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">000149</idno></publicationStmt><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></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><mods:affiliation>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: mariapia.dimauro@iasf‐roma.inaf.it</mods:affiliation></affiliation></author><author><name sortKey="Cardini, D" sort="Cardini, D" uniqKey="Cardini D" first="D." last="Cardini">D. Cardini</name><affiliation><mods:affiliation>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy</mods:affiliation></affiliation></author><author><name sortKey="Catanzaro, G" sort="Catanzaro, G" uniqKey="Catanzaro G" first="G." last="Catanzaro">G. Catanzaro</name><affiliation><mods:affiliation>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</mods:affiliation></affiliation></author><author><name sortKey="Ventura, R" sort="Ventura, R" uniqKey="Ventura R" first="R." last="Ventura">R. Ventura</name><affiliation><mods:affiliation>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</mods:affiliation></affiliation></author><author><name sortKey="Barban, C" sort="Barban, C" uniqKey="Barban C" first="C." last="Barban">C. Barban</name><affiliation><mods:affiliation>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France</mods:affiliation></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><mods:affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation></author><author><name sortKey="Christensen Alsgaard, J" sort="Christensen Alsgaard, J" uniqKey="Christensen Alsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name><affiliation><mods:affiliation>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark</mods:affiliation></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><mods:affiliation>Institut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium</mods:affiliation></affiliation></author><author><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name><affiliation><mods:affiliation>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</mods:affiliation></affiliation><affiliation><mods:affiliation>Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands</mods:affiliation></affiliation></author><author><name sortKey="Huber, D" sort="Huber, D" uniqKey="Huber D" first="D." last="Huber">D. Huber</name><affiliation><mods:affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation></author><author><name sortKey="Kallinger, T" sort="Kallinger, T" uniqKey="Kallinger T" first="T." last="Kallinger">T. Kallinger</name><affiliation><mods:affiliation>Department of Physics and Astronomy, University of British Columbia, Vancouver, Canada</mods:affiliation></affiliation><affiliation><mods:affiliation>Institute of Astronomy, University of Vienna, 1180 Vienna, Austria</mods:affiliation></affiliation></author><author><name sortKey="Miglio, A" sort="Miglio, A" uniqKey="Miglio A" first="A." last="Miglio">A. Miglio</name><affiliation><mods:affiliation>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</mods:affiliation></affiliation><affiliation><mods:affiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</mods:affiliation></affiliation></author><author><name sortKey="Montalban, J" sort="Montalban, J" uniqKey="Montalban J" first="J." last="Montalban">J. Montalban</name><affiliation><mods:affiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</mods:affiliation></affiliation></author><author><name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name><affiliation><mods:affiliation>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France</mods:affiliation></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation><mods:affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation></author><author><name sortKey="Uytterhoeven, K" sort="Uytterhoeven, K" uniqKey="Uytterhoeven K" first="K." last="Uytterhoeven">K. Uytterhoeven</name><affiliation><mods:affiliation>Laboratoire AIM, CEA/DSM‐CNRS‐Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay, 91191 Gif‐sur‐Yvette, France</mods:affiliation></affiliation><affiliation><mods:affiliation>Kiepenheuer‐Institut für Sonnenphysik, Schöneckstraße 6, 79104 Freiburg im Breisgau, Germany</mods:affiliation></affiliation></author><author><name sortKey="Kinemuchi, K" sort="Kinemuchi, K" uniqKey="Kinemuchi K" first="K." last="Kinemuchi">K. Kinemuchi</name><affiliation><mods:affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation><mods:affiliation>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark</mods:affiliation></affiliation></author><author><name sortKey="Mullally, F" sort="Mullally, F" uniqKey="Mullally F" first="F." last="Mullally">F. Mullally</name><affiliation><mods:affiliation>SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation></affiliation></author><author><name sortKey="Still, M" sort="Still, M" uniqKey="Still M" first="M." last="Still">M. Still</name><affiliation><mods:affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</mods:affiliation></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></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><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><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>convective</json:string><json:string>convective envelope</json:string><json:string>mnras</json:string><json:string>kjeldsen</json:string><json:string>monthly notices</json:string><json:string>effective temperature</json:string><json:string>kallinger</json:string><json:string>power spectrum</json:string><json:string>miglio</json:string><json:string>mosser</json:string><json:string>stellar</json:string><json:string>rotational</json:string><json:string>radial modes</json:string><json:string>mauro</json:string><json:string>oscillation</json:string><json:string>radial order</json:string><json:string>echelle</json:string><json:string>astron</json:string><json:string>adiabatic</json:string><json:string>overshooting</json:string><json:string>oscillation spectrum</json:string><json:string>tting</json:string><json:string>kepler</json:string><json:string>ionization</json:string><json:string>huber</json:string><json:string>turbulent diffusion</json:string><json:string>tted</json:string><json:string>oscillation frequencies</json:string><json:string>spectroscopic</json:string><json:string>hekker</json:string><json:string>harmonic degree</json:string><json:string>large frequency separation</json:string><json:string>power density spectrum</json:string><json:string>acoustic</json:string><json:string>large separation</json:string><json:string>free parameters</json:string><json:string>acoustic modes</json:string><json:string>buoyancy frequency</json:string><json:string>frequency range</json:string><json:string>echelle diagram</json:string><json:string>luminosity</json:string><json:string>mode</json:string><json:string>bedding</json:string><json:string>evolutionary state</json:string><json:string>frequency resolution</json:string><json:string>sharp variation</json:string><json:string>period spacings</json:string><json:string>mcdonald observatory</json:string><json:string>open symbols</json:string><json:string>oscillation modes</json:string><json:string>rotational splittings</json:string><json:string>kepler satellite</json:string><json:string>inertia</json:string><json:string>atmospheric parameters</json:string><json:string>high frequencies</json:string><json:string>bedding kjeldsen</json:string><json:string>stellar background</json:string><json:string>individual frequencies</json:string><json:string>white noise</json:string><json:string>maximum amplitude</json:string><json:string>radial mode</json:string><json:string>nancial support</json:string><json:string>stellar structure</json:string><json:string>second ionization</json:string><json:string>integration time</json:string><json:string>solid lines</json:string><json:string>lamb frequencies</json:string><json:string>mode width</json:string><json:string>high inertia</json:string><json:string>echelle diagrams</json:string><json:string>iron abundance</json:string><json:string>rotational splitting</json:string><json:string>bottom panel</json:string><json:string>parameter</json:string><json:string>frequency</json:string><json:string>radial</json:string><json:string>main parameters</json:string><json:string>straight line</json:string><json:string>unprecedented level</json:string><json:string>oscillatory signal</json:string><json:string>spectral window</json:string><json:string>light curve</json:string><json:string>mode degree</json:string><json:string>oscillation spectra</json:string><json:string>spectroscopic observations</json:string><json:string>standard deviation</json:string><json:string>envelope autocorrelation function analysis</json:string><json:string>mosser appourchaux</json:string><json:string>abundance pattern</json:string><json:string>small frequency separation</json:string><json:string>small separation</json:string><json:string>stellar activity</json:string><json:string>mode lifetime</json:string><json:string>small frequency separations</json:string><json:string>central frequency</json:string><json:string>independent averages</json:string><json:string>other parameters</json:string><json:string>stellar spectrum</json:string><json:string>good agreement</json:string><json:string>kjeldsen bedding</json:string><json:string>global asteroseismic parameters</json:string><json:string>lled symbols</json:string><json:string>surface gravity</json:string><json:string>photon noise</json:string><json:string>pressure scaleheight</json:string><json:string>atlas9 code</json:string><json:string>evolutionary phase</json:string><json:string>oscillation properties</json:string><json:string>upper panel</json:string><json:string>lower panel</json:string><json:string>initial hydrogen abundance</json:string><json:string>additional effects</json:string><json:string>spectroscopic constraints</json:string><json:string>acoustical frequency</json:string><json:string>grey dots</json:string><json:string>prevalent character</json:string><json:string>adiabatic frequencies</json:string><json:string>regular spacing</json:string><json:string>effective temperature ranges</json:string><json:string>vertical line</json:string><json:string>propagation diagram</json:string><json:string>hydrogen abundance</json:string><json:string>similar frequencies</json:string><json:string>same frequency</json:string><json:string>strong character</json:string><json:string>gravity character</json:string><json:string>blue triangles</json:string><json:string>gravity waves</json:string><json:string>direct modelling</json:string><json:string>acoustic waves</json:string><json:string>results show</json:string><json:string>relative surface amplitude</json:string><json:string>lower frequencies</json:string><json:string>theoretical frequencies</json:string><json:string>allende prieto</json:string><json:string>present analysis</json:string><json:string>moffett field</json:string><json:string>acoustic radius</json:string><json:string>sharp features</json:string><json:string>publications division</json:string><json:string>cambridge univ</json:string><json:string>window function</json:string><json:string>theoretical models</json:string><json:string>binned power spectrum</json:string><json:string>small separations</json:string><json:string>background model</json:string><json:string>thermodynamic properties</json:string><json:string>harmonic</json:string><json:string>spectrum</json:string></teeft></keywords><author><json:item><name>M. P. Di Mauro</name><affiliations><json:string>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy</json:string><json:string>E-mail: mariapia.dimauro@iasf‐roma.inaf.it</json:string></affiliations></json:item><json:item><name>D. Cardini</name><affiliations><json:string>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy</json:string></affiliations></json:item><json:item><name>G. Catanzaro</name><affiliations><json:string>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</json:string></affiliations></json:item><json:item><name>R. Ventura</name><affiliations><json:string>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</json:string></affiliations></json:item><json:item><name>C. Barban</name><affiliations><json:string>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France</json:string></affiliations></json:item><json:item><name>T. R. Bedding</name><affiliations><json:string>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>J. Christensen‐Dalsgaard</name><affiliations><json:string>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark</json:string></affiliations></json:item><json:item><name>J. De Ridder</name><affiliations><json:string>Institut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium</json:string></affiliations></json:item><json:item><name>S. Hekker</name><affiliations><json:string>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</json:string><json:string>Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands</json:string></affiliations></json:item><json:item><name>D. Huber</name><affiliations><json:string>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>T. Kallinger</name><affiliations><json:string>Department of Physics and Astronomy, University of British Columbia, Vancouver, Canada</json:string><json:string>Institute of Astronomy, University of Vienna, 1180 Vienna, Austria</json:string></affiliations></json:item><json:item><name>A. Miglio</name><affiliations><json:string>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</json:string><json:string>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</json:string></affiliations></json:item><json:item><name>J. Montalban</name><affiliations><json:string>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</json:string></affiliations></json:item><json:item><name>B. Mosser</name><affiliations><json:string>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France</json:string></affiliations></json:item><json:item><name>D. Stello</name><affiliations><json:string>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>K. Uytterhoeven</name><affiliations><json:string>Laboratoire AIM, CEA/DSM‐CNRS‐Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay, 91191 Gif‐sur‐Yvette, France</json:string><json:string>Kiepenheuer‐Institut für Sonnenphysik, Schöneckstraße 6, 79104 Freiburg im Breisgau, Germany</json:string></affiliations></json:item><json:item><name>K. Kinemuchi</name><affiliations><json:string>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</json:string></affiliations></json:item><json:item><name>H. Kjeldsen</name><affiliations><json:string>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark</json:string></affiliations></json:item><json:item><name>F. Mullally</name><affiliations><json:string>SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</json:string></affiliations></json:item><json:item><name>M. Still</name><affiliations><json:string>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>stars: AGB and post‐AGB</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>stars: evolution</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>stars: fundamental parameters</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>stars: individual: KIC 4351319</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>stars: oscillations</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>stars: solar‐type</value></json:item></subject><articleId><json:string>MNR18996</json:string></articleId><arkIstex>ark:/67375/WNG-RJ3KTLRP-L</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><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.</abstract><qualityIndicators><score>9.64</score><pdfWordCount>11257</pdfWordCount><pdfCharCount>60638</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>15</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>220</abstractWordCount><abstractCharCount>1484</abstractCharCount><keywordCount>6</keywordCount></qualityIndicators><title>Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>415</volume><issue>4</issue><pages><first>3783</first><last>3797</last><total>15</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2011</json:string><json:string>8497</json:string></date><geogName></geogName><orgName><json:string>University of Birmingham</json:string><json:string>University of Amsterdam</json:string><json:string>University of Sydney</json:string><json:string>Department of Physics and Astronomy</json:string><json:string>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA</json:string><json:string>University of British Columbia</json:string><json:string>SETI Institute/NASA Ames Research Center, Moffett Field, CA</json:string><json:string>Cr Mn Fe Co</json:string><json:string>Netherlands Organization for Scienti</json:string><json:string>ESA</json:string><json:string>UK Science and Technology</json:string><json:string>Canadian Space Agency</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>H. Kjeldsen</json:string><json:string>Craig B. Markwardt</json:string><json:string>K. Uytterhoeven</json:string><json:string>D. Huber</json:string><json:string>S. Hekker</json:string><json:string>D. Stello</json:string><json:string>Harlan J. Smith</json:string><json:string>D. Cardini</json:string><json:string>Paris Diderot</json:string><json:string>Marie Curie</json:string><json:string>A. Miglio</json:string><json:string>The</json:string><json:string>M. P. Di Mauro</json:string><json:string>F. Mullally</json:string><json:string>Smith Telescope</json:string><json:string>K. Kinemuchi</json:string><json:string>Anton Pannekoek</json:string><json:string>Ny Munkegade</json:string></persName><placeName><json:string>Birmingham</json:string><json:string>Germany</json:string><json:string>Australia</json:string><json:string>Opacity</json:string><json:string>Meudon</json:string><json:string>Austria</json:string><json:string>Canada</json:string><json:string>Freiburg im Breisgau</json:string><json:string>Vancouver</json:string><json:string>Strasbourg</json:string><json:string>Vienna</json:string><json:string>Amsterdam</json:string><json:string>Denmark</json:string><json:string>Gif-sur-Yvette</json:string><json:string>Leuven</json:string><json:string>France</json:string><json:string>Italy</json:string><json:string>Catania</json:string><json:string>Belgium</json:string><json:string>Netherlands</json:string></placeName><ref_url><json:string>http://archive.stsci.edu/kepler/kepler_fov/search.php</json:string><json:string>http://cow.physics.wisc.edu/</json:string><json:string>http://simbad.u-strasbg.fr/simbad/</json:string></ref_url><ref_bibl><json:string>Bedding et al. 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(2011a)</json:string><json:string>De Ridder et al. 2009</json:string><json:string>Milne 1926</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-RJ3KTLRP-L</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences biologiques et medicales</json:string><json:string>3 - sciences biologiques fondamentales et appliquees. psychologie</json:string></inist></categories><publicationDate>2011</publicationDate><copyrightDate>2011</copyrightDate><doi><json:string>10.1111/j.1365-2966.2011.18996.x</json:string></doi><id>07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C/fulltext/tei"><teiHeader><fileDesc><titleStmt><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></title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</licence></availability><date type="published" when="2011-08-21"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><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></title><title level="a" type="short">Solar‐like oscillations of KIC 4351319</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">M. P.</forename><surname>Di Mauro</surname></persName><affiliation>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy<address><country key="IT"></country></address></affiliation><affiliation>E‐mail: mariapia.dimauro@iasf‐roma.inaf.it</affiliation></author><author xml:id="author-0001"><persName><forename type="first">D.</forename><surname>Cardini</surname></persName><affiliation>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">G.</forename><surname>Catanzaro</surname></persName><affiliation>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">R.</forename><surname>Ventura</surname></persName><affiliation>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">C.</forename><surname>Barban</surname></persName><affiliation>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">T. R.</forename><surname>Bedding</surname></persName><affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">J.</forename><surname>Christensen‐Dalsgaard</surname></persName><affiliation>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark<address><country key="DK"></country></address></affiliation></author><author xml:id="author-0007"><persName><forename type="first">J.</forename><surname>De Ridder</surname></persName><affiliation>Institut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium<address><country key="BE"></country></address></affiliation></author><author xml:id="author-0008"><persName><forename type="first">S.</forename><surname>Hekker</surname></persName><affiliation>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</affiliation><affiliation>Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands<address><country key="NL"></country></address></affiliation></author><author xml:id="author-0009"><persName><forename type="first">D.</forename><surname>Huber</surname></persName><affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0010"><persName><forename type="first">T.</forename><surname>Kallinger</surname></persName><affiliation>Department of Physics and Astronomy, University of British Columbia, Vancouver, Canada<address><country key="CA"></country></address></affiliation><affiliation>Institute of Astronomy, University of Vienna, 1180 Vienna, Austria<address><country key="AT"></country></address></affiliation></author><author xml:id="author-0011"><persName><forename type="first">A.</forename><surname>Miglio</surname></persName><affiliation>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</affiliation><affiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium<address><country key="BE"></country></address></affiliation></author><author xml:id="author-0012"><persName><forename type="first">J.</forename><surname>Montalban</surname></persName><affiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium<address><country key="BE"></country></address></affiliation></author><author xml:id="author-0013"><persName><forename type="first">B.</forename><surname>Mosser</surname></persName><affiliation>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0014"><persName><forename type="first">D.</forename><surname>Stello</surname></persName><affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0015"><persName><forename type="first">K.</forename><surname>Uytterhoeven</surname></persName><affiliation>Laboratoire AIM, CEA/DSM‐CNRS‐Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay, 91191 Gif‐sur‐Yvette, France<address><country key="FR"></country></address></affiliation><affiliation>Kiepenheuer‐Institut für Sonnenphysik, Schöneckstraße 6, 79104 Freiburg im Breisgau, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0016"><persName><forename type="first">K.</forename><surname>Kinemuchi</surname></persName><affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0017"><persName><forename type="first">H.</forename><surname>Kjeldsen</surname></persName><affiliation>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark<address><country key="DK"></country></address></affiliation></author><author xml:id="author-0018"><persName><forename type="first">F.</forename><surname>Mullally</surname></persName><affiliation>SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0019"><persName><forename type="first">M.</forename><surname>Still</surname></persName><affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA<address><country key="US"></country></address></affiliation></author><idno type="istex">07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C</idno><idno type="ark">ark:/67375/WNG-RJ3KTLRP-L</idno><idno type="DOI">10.1111/j.1365-2966.2011.18996.x</idno><idno type="unit">MNR18996</idno><idno type="toTypesetVersion">file:MNR.MNR18996.pdf</idno></analytic><monogr><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="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="book-DOI">10.1111/(ISSN)1365-2966</idno><idno type="book-part-DOI">10.1111/mnr.2011.415.issue-4</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</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"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>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 <hi rend="italic">Kepler</hi> satellite. The analysis has allowed us to determine the large and small frequency separations, <graphic url="equation/MNR_18996_mu1.gif" rend="inline image"></graphic>Hz and <graphic url="equation/MNR_18996_mu2.gif" rend="inline image"></graphic>Hz, respectively, and the frequency of maximum oscillation power, <graphic url="equation/MNR_18996_mu3.gif" rend="inline image"></graphic>Hz.</p><p>The high signal‐to‐noise ratio of the observations allowed us to identify 25 independent pulsation modes whose frequencies range approximately from 300 to <graphic url="equation/MNR_18996_mu4.gif" rend="inline image"></graphic>Hz.</p><p>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.</p><p>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.</p><p>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<hi rend="subscript">⊙</hi>, a radius of <graphic url="equation/MNR_18996_mu5.gif" rend="inline image"></graphic> 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.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">stars: AGB and post‐AGB</term><term xml:id="k2">stars: evolution</term><term xml:id="k3">stars: fundamental parameters</term><term xml:id="k4">stars: individual: KIC 4351319</term><term xml:id="k5">stars: oscillations</term><term xml:id="k6">stars: solar‐type</term></keywords><keywords rend="tocHeading1"><term>Papers</term></keywords></textClass><langUsage><language ident="en"></language></langUsage></profileDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi><issn type="print">0035-8711</issn><issn type="electronic">1365-2966</issn><idGroup><id type="product" value="MNR"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title></titleGroup></publicationMeta><publicationMeta level="part" position="08104"><doi origin="wiley">10.1111/mnr.2011.415.issue-4</doi><numberingGroup><numbering type="journalVolume" number="415">415</numbering><numbering type="journalIssue" number="4">4</numbering></numberingGroup><coverDate startDate="2011-08-21">August 2011</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="70" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2011.18996.x</doi><idGroup><id type="unit" value="MNR18996"></id></idGroup><countGroup><count type="pageTotal" number="15"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</copyright><eventGroup><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.9.1 mode:FullText" date="2011-08-19"></event><event type="publishedOnlineEarlyUnpaginated" date="2011-07-26"></event><event type="publishedOnlineFinalForm" date="2011-08-18"></event><event type="firstOnline" date="2011-07-26"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-03"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-10-31"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="3783">3783</numbering><numbering type="pageLast" number="3797">3797</numbering></numberingGroup><correspondenceTo>
E‐mail: <email normalForm="mariapia.dimauro@iasf-roma.inaf.it">mariapia.dimauro@iasf‐roma.inaf.it</email></correspondenceTo><objectNameGroup><objectName elementName="appendix">Appendices</objectName></objectNameGroup><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR18996.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2011 May 2. Received 2011 May 2; in original form 2011 January 10</unparsedEditorialHistory><countGroup><count type="figureTotal" number="16"></count><count type="tableTotal" number="4"></count><count type="formulaTotal" number="73"></count><count type="referenceTotal" number="90"></count><count type="linksCrossRef" number="217"></count></countGroup><titleGroup><title type="main">Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with <i>Kepler</i></title><title type="shortAuthors"><i>M. P. Di Mauro et al.</i></title><title type="short"><i>Solar‐like oscillations of KIC 4351319</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>M. P.</givenNames><familyName>Di Mauro</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a1"><personName><givenNames>D.</givenNames><familyName>Cardini</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a2"><personName><givenNames>G.</givenNames><familyName>Catanzaro</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a2"><personName><givenNames>R.</givenNames><familyName>Ventura</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a3"><personName><givenNames>C.</givenNames><familyName>Barban</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a4"><personName><givenNames>T. R.</givenNames><familyName>Bedding</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a5"><personName><givenNames>J.</givenNames><familyName>Christensen‐Dalsgaard</familyName></personName></creator><creator creatorRole="author" xml:id="cr8" affiliationRef="#a6"><personName><givenNames>J.</givenNames><familyName>De Ridder</familyName></personName></creator><creator creatorRole="author" xml:id="cr9" affiliationRef="#a7 #a8"><personName><givenNames>S.</givenNames><familyName>Hekker</familyName></personName></creator><creator creatorRole="author" xml:id="cr10" affiliationRef="#a4"><personName><givenNames>D.</givenNames><familyName>Huber</familyName></personName></creator><creator creatorRole="author" xml:id="cr11" affiliationRef="#a9 #a10"><personName><givenNames>T.</givenNames><familyName>Kallinger</familyName></personName></creator><creator creatorRole="author" xml:id="cr12" affiliationRef="#a7 #a11"><personName><givenNames>A.</givenNames><familyName>Miglio</familyName></personName></creator><creator creatorRole="author" xml:id="cr13" affiliationRef="#a11"><personName><givenNames>J.</givenNames><familyName>Montalban</familyName></personName></creator><creator creatorRole="author" xml:id="cr14" affiliationRef="#a3"><personName><givenNames>B.</givenNames><familyName>Mosser</familyName></personName></creator><creator creatorRole="author" xml:id="cr15" affiliationRef="#a4"><personName><givenNames>D.</givenNames><familyName>Stello</familyName></personName></creator><creator creatorRole="author" xml:id="cr16" affiliationRef="#a12 #a13"><personName><givenNames>K.</givenNames><familyName>Uytterhoeven</familyName></personName></creator><creator creatorRole="author" xml:id="cr17" affiliationRef="#a14"><personName><givenNames>K.</givenNames><familyName>Kinemuchi</familyName></personName></creator><creator creatorRole="author" xml:id="cr18" affiliationRef="#a5"><personName><givenNames>H.</givenNames><familyName>Kjeldsen</familyName></personName></creator><creator creatorRole="author" xml:id="cr19" affiliationRef="#a15"><personName><givenNames>F.</givenNames><familyName>Mullally</familyName></personName></creator><creator creatorRole="author" xml:id="cr20" affiliationRef="#a14"><personName><givenNames>M.</givenNames><familyName>Still</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="IT"><unparsedAffiliation>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="IT"><unparsedAffiliation>INAF – Osservatorio Astrofisico di Catania, Via S. 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Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium</unparsedAffiliation></affiliation><affiliation xml:id="a7"><unparsedAffiliation>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</unparsedAffiliation></affiliation><affiliation xml:id="a8" countryCode="NL"><unparsedAffiliation>Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands</unparsedAffiliation></affiliation><affiliation xml:id="a9" countryCode="CA"><unparsedAffiliation>Department of Physics and Astronomy, University of British Columbia, Vancouver, Canada</unparsedAffiliation></affiliation><affiliation xml:id="a10" countryCode="AT"><unparsedAffiliation>Institute of Astronomy, University of Vienna, 1180 Vienna, Austria</unparsedAffiliation></affiliation><affiliation xml:id="a11" countryCode="BE"><unparsedAffiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</unparsedAffiliation></affiliation><affiliation xml:id="a12" countryCode="FR"><unparsedAffiliation>Laboratoire AIM, CEA/DSM‐CNRS‐Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay, 91191 Gif‐sur‐Yvette, France</unparsedAffiliation></affiliation><affiliation xml:id="a13" countryCode="DE"><unparsedAffiliation>Kiepenheuer‐Institut für Sonnenphysik, Schöneckstraße 6, 79104 Freiburg im Breisgau, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a14" countryCode="US"><unparsedAffiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</unparsedAffiliation></affiliation><affiliation xml:id="a15" countryCode="US"><unparsedAffiliation>SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">stars: AGB and post‐AGB</keyword><keyword xml:id="k2">stars: evolution</keyword><keyword xml:id="k3">stars: fundamental parameters</keyword><keyword xml:id="k4">stars: individual: KIC 4351319</keyword><keyword xml:id="k5">stars: oscillations</keyword><keyword xml:id="k6">stars: solar‐type</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>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 <i>Kepler</i> satellite. The analysis has allowed us to determine the large and small frequency separations, <inlineGraphic alt="inline image" location="equation/MNR_18996_mu1.gif" href=""></inlineGraphic>Hz and <inlineGraphic alt="inline image" location="equation/MNR_18996_mu2.gif" href=""></inlineGraphic>Hz, respectively, and the frequency of maximum oscillation power, <inlineGraphic alt="inline image" location="equation/MNR_18996_mu3.gif" href=""></inlineGraphic>Hz.</p><p>The high signal‐to‐noise ratio of the observations allowed us to identify 25 independent pulsation modes whose frequencies range approximately from 300 to <inlineGraphic alt="inline image" location="equation/MNR_18996_mu4.gif" href=""></inlineGraphic>Hz.</p><p>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.</p><p>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.</p><p>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<sub>⊙</sub>, a radius of <inlineGraphic alt="inline image" location="equation/MNR_18996_mu5.gif" href=""></inlineGraphic> 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.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Solar‐like oscillations of KIC 4351319</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler</title></titleInfo><name type="personal"><namePart type="given">M. P.</namePart><namePart type="family">Di Mauro</namePart><affiliation>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy</affiliation><affiliation>E-mail: mariapia.dimauro@iasf‐roma.inaf.it</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Cardini</namePart><affiliation>INAF – IASF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G.</namePart><namePart type="family">Catanzaro</namePart><affiliation>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.</namePart><namePart type="family">Ventura</namePart><affiliation>INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C.</namePart><namePart type="family">Barban</namePart><affiliation>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T. R.</namePart><namePart type="family">Bedding</namePart><affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Christensen‐Dalsgaard</namePart><affiliation>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">De Ridder</namePart><affiliation>Institut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">Hekker</namePart><affiliation>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</affiliation><affiliation>Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Huber</namePart><affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T.</namePart><namePart type="family">Kallinger</namePart><affiliation>Department of Physics and Astronomy, University of British Columbia, Vancouver, Canada</affiliation><affiliation>Institute of Astronomy, University of Vienna, 1180 Vienna, Austria</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Miglio</namePart><affiliation>School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT</affiliation><affiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Montalban</namePart><affiliation>Institut d’Astrophysique et de Géofisique de l’Universitè de Liège, Allè du 6 Aout 17‐B 4000 Liège, Belgium</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">B.</namePart><namePart type="family">Mosser</namePart><affiliation>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris, 92195 Meudon Cedex, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Stello</namePart><affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">K.</namePart><namePart type="family">Uytterhoeven</namePart><affiliation>Laboratoire AIM, CEA/DSM‐CNRS‐Université Paris Diderot, CEA, IRFU, SAp, Centre de Saclay, 91191 Gif‐sur‐Yvette, France</affiliation><affiliation>Kiepenheuer‐Institut für Sonnenphysik, Schöneckstraße 6, 79104 Freiburg im Breisgau, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">K.</namePart><namePart type="family">Kinemuchi</namePart><affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">H.</namePart><namePart type="family">Kjeldsen</namePart><affiliation>Institut for Fysik og Astronomi, Bygn. 1520, Aarhus Universitet, Ny Munkegade, DK‐8000 Aarhus C, Denmark</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">F.</namePart><namePart type="family">Mullally</namePart><affiliation>SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Still</namePart><affiliation>Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2011-08-21</dateIssued><edition>Accepted 2011 May 2. Received 2011 May 2; in original form 2011 January 10</edition><copyrightDate encoding="w3cdtf">2011</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">16</extent><extent unit="tables">4</extent><extent unit="formulas">73</extent><extent unit="references">90</extent><extent unit="linksCrossRef">217</extent></physicalDescription><abstract 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.</abstract><subject lang="en"><genre>keywords</genre><topic>stars: AGB and post‐AGB</topic><topic>stars: evolution</topic><topic>stars: fundamental parameters</topic><topic>stars: individual: KIC 4351319</topic><topic>stars: oscillations</topic><topic>stars: solar‐type</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2011</date><detail type="volume"><caption>vol.</caption><number>415</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>3783</start><end>3797</end><total>15</total></extent></part></relatedItem><identifier type="istex">07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C</identifier><identifier type="ark">ark:/67375/WNG-RJ3KTLRP-L</identifier><identifier type="DOI">10.1111/j.1365-2966.2011.18996.x</identifier><identifier type="ArticleID">MNR18996</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</accessCondition><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/07BE3F2CCF5C06BE96E33B9BFBA85A834D23251C/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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