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
Links to Exploration step
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<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>
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<affiliation><mods:affiliation>E-mail: mariapia.dimauro@iasf‐roma.inaf.it</mods:affiliation>
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<author><name sortKey="Cardini, D" sort="Cardini, D" uniqKey="Cardini D" first="D." last="Cardini">D. Cardini</name>
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<author><name sortKey="Catanzaro, G" sort="Catanzaro, G" uniqKey="Catanzaro G" first="G." last="Catanzaro">G. Catanzaro</name>
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<author><name sortKey="Ventura, R" sort="Ventura, R" uniqKey="Ventura R" first="R." last="Ventura">R. Ventura</name>
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<author><name sortKey="Barban, C" sort="Barban, C" uniqKey="Barban C" first="C." last="Barban">C. Barban</name>
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<author><name sortKey="Bedding, T R" sort="Bedding, T R" uniqKey="Bedding T" first="T. R." last="Bedding">T. R. Bedding</name>
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<author><name sortKey="Christensen Alsgaard, J" sort="Christensen Alsgaard, J" uniqKey="Christensen Alsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name>
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<author><name sortKey="De Ridder, J" sort="De Ridder, J" uniqKey="De Ridder J" first="J." last="De Ridder">J. De Ridder</name>
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<author><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name>
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<author><name sortKey="Huber, D" sort="Huber, D" uniqKey="Huber D" first="D." last="Huber">D. Huber</name>
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<affiliation><mods:affiliation>Institute of Astronomy, University of Vienna, 1180 Vienna, Austria</mods:affiliation>
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<author><name sortKey="Miglio, A" sort="Miglio, A" uniqKey="Miglio A" first="A." last="Miglio">A. Miglio</name>
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<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>
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<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>
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<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>
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<author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name>
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</affiliation>
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<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>
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<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>
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<author><name sortKey="Still, M" sort="Still, M" uniqKey="Still M" first="M." last="Still">M. Still</name>
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<sourceDesc><biblStruct><analytic><title level="a" type="main">Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with <hi rend="italic">Kepler</hi>
</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>
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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Abundance pattern</term>
<term>Acoustic</term>
<term>Acoustic modes</term>
<term>Acoustic radius</term>
<term>Acoustic waves</term>
<term>Acoustical frequency</term>
<term>Additional effects</term>
<term>Adiabatic</term>
<term>Adiabatic frequencies</term>
<term>Allende prieto</term>
<term>Astron</term>
<term>Atlas9 code</term>
<term>Atmospheric parameters</term>
<term>Background model</term>
<term>Bedding</term>
<term>Bedding kjeldsen</term>
<term>Binned power spectrum</term>
<term>Blue triangles</term>
<term>Bottom panel</term>
<term>Buoyancy frequency</term>
<term>Cambridge univ</term>
<term>Central frequency</term>
<term>Convective</term>
<term>Convective envelope</term>
<term>Direct modelling</term>
<term>Echelle</term>
<term>Echelle diagram</term>
<term>Echelle diagrams</term>
<term>Effective temperature</term>
<term>Effective temperature ranges</term>
<term>Envelope autocorrelation function analysis</term>
<term>Evolutionary phase</term>
<term>Evolutionary state</term>
<term>Free parameters</term>
<term>Frequency</term>
<term>Frequency range</term>
<term>Frequency resolution</term>
<term>Global asteroseismic parameters</term>
<term>Good agreement</term>
<term>Gravity character</term>
<term>Gravity waves</term>
<term>Grey dots</term>
<term>Harmonic</term>
<term>Harmonic degree</term>
<term>Hekker</term>
<term>High frequencies</term>
<term>High inertia</term>
<term>Huber</term>
<term>Hydrogen abundance</term>
<term>Independent averages</term>
<term>Individual frequencies</term>
<term>Inertia</term>
<term>Initial hydrogen abundance</term>
<term>Integration time</term>
<term>Ionization</term>
<term>Iron abundance</term>
<term>Kallinger</term>
<term>Kepler</term>
<term>Kepler satellite</term>
<term>Kjeldsen</term>
<term>Kjeldsen bedding</term>
<term>Lamb frequencies</term>
<term>Large frequency separation</term>
<term>Large separation</term>
<term>Light curve</term>
<term>Lled symbols</term>
<term>Lower frequencies</term>
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<term>Spectroscopic observations</term>
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<term>Acoustical frequency</term>
<term>Additional effects</term>
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<term>Echelle diagram</term>
<term>Echelle diagrams</term>
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<term>Mode degree</term>
<term>Mode lifetime</term>
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<term>Mosser appourchaux</term>
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<term>Publications division</term>
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<term>Radial modes</term>
<term>Radial order</term>
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<term>Rotational splittings</term>
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<term>Second ionization</term>
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<term>Spectroscopic</term>
<term>Spectroscopic constraints</term>
<term>Spectroscopic observations</term>
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<term>Standard deviation</term>
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<term>Stellar activity</term>
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<term>Stellar spectrum</term>
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<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>
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<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>
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<json:item><name>D. Cardini</name>
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<json:item><name>C. Barban</name>
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<json:item><name>T. R. Bedding</name>
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<json:item><name>J. Christensen‐Dalsgaard</name>
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<json:item><name>T. Kallinger</name>
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<json:string>Institute of Astronomy, University of Vienna, 1180 Vienna, Austria</json:string>
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<json:item><name>A. Miglio</name>
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<json:item><name>J. Montalban</name>
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<json:item><name>B. Mosser</name>
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<json:item><name>D. Stello</name>
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<json:item><name>K. Uytterhoeven</name>
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<json:item><name>M. Still</name>
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<value>stars: AGB and post‐AGB</value>
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<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>
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<title>Solar‐like oscillations from the depths of the red‐giant star KIC 4351319 observed with Kepler</title>
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<author xml:id="author-0004"><persName><forename type="first">C.</forename>
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<author xml:id="author-0005"><persName><forename type="first">T. R.</forename>
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<affiliation>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia<address><country key="AU"></country>
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<author xml:id="author-0006"><persName><forename type="first">J.</forename>
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<author xml:id="author-0007"><persName><forename type="first">J.</forename>
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<affiliation>Institut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium<address><country key="BE"></country>
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<author xml:id="author-0008"><persName><forename type="first">S.</forename>
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<author xml:id="author-0009"><persName><forename type="first">D.</forename>
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<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>
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<term xml:id="k4">stars: individual: KIC 4351319</term>
<term xml:id="k5">stars: oscillations</term>
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<title type="short"><i>Solar‐like oscillations of KIC 4351319</i>
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<keyword xml:id="k4">stars: individual: KIC 4351319</keyword>
<keyword xml:id="k5">stars: oscillations</keyword>
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<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>
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<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>
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<topic>stars: AGB and post‐AGB</topic>
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<topic>stars: fundamental parameters</topic>
<topic>stars: individual: KIC 4351319</topic>
<topic>stars: oscillations</topic>
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