MODELING KEPLER OBSERVATIONS OF SOLAR-LIKE OSCILLATIONS IN THE RED GIANT STAR HD 186355
Identifieur interne : 004797 ( PascalFrancis/Curation ); précédent : 004796; suivant : 004798MODELING KEPLER OBSERVATIONS OF SOLAR-LIKE OSCILLATIONS IN THE RED GIANT STAR HD 186355
Auteurs : C. Jiang [République populaire de Chine] ; B. W. Jiang [République populaire de Chine] ; J. Christensen-Dalsgaard [Danemark] ; T. R. Bedding [Australie] ; D. Stello [Australie] ; D. Huber [Australie] ; S. Frandsen [Danemark] ; H. Kjeldsen [Danemark] ; C. Karoff [Danemark] ; B. Mosser [France] ; P. Demarque [États-Unis] ; M. N. Fanelli [États-Unis] ; K. Kinemuchi [États-Unis] ; F. Mullally [États-Unis]Source :
- The Astrophysical journal [ 0004-637X ] ; 2011.
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Abstract
We have analyzed oscillations of the red giant star HD 186355 observed by the NASA Kepler satellite. The data consist of the first five quarters of science operations of Kepler, which cover about 13 months. The high-precision time-series data allow us to accurately extract the oscillation frequencies from the power spectrum. We find that the frequency of the maximum oscillation power, νmax, and the mean large frequency separation, Δν, are around 106 and 9.4 μHz, respectively. A regular pattern of radial and non-radial oscillation modes is identified by stacking the power spectra in an echelle diagram. We use the scaling relations of Δν and νmax to estimate the preliminary asteroseismic mass, which is confirmed with the modeling result (M = 1.45 ± 0.05 M◦.) using the Yale Rotating stellar Evolution Code (YREC7). In addition, we constrain the effective temperature, luminosity, and radius from comparisons between observational constraints and models. A number of mixed l = 1 modes are also detected and taken into account in our model comparisons. We find a mean observational period spacing for these mixed modes of about 58 s, suggesting that this red giant branch star is in the shell hydrogen-burning phase.
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<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">MODELING KEPLER OBSERVATIONS OF SOLAR-LIKE OSCILLATIONS IN THE RED GIANT STAR HD 186355</title><author><name sortKey="Jiang, C" sort="Jiang, C" uniqKey="Jiang C" first="C." last="Jiang">C. Jiang</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Astronomy, Beijing Normal University</s1><s2>Beijing 100875</s2><s3>CHN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>République populaire de Chine</country></affiliation></author><author><name sortKey="Jiang, B W" sort="Jiang, B W" uniqKey="Jiang B" first="B. W." last="Jiang">B. W. Jiang</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Astronomy, Beijing Normal University</s1><s2>Beijing 100875</s2><s3>CHN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>République populaire de Chine</country></affiliation></author><author><name sortKey="Christensen Dalsgaard, J" sort="Christensen Dalsgaard, J" uniqKey="Christensen Dalsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Bedding, T R" sort="Bedding, T R" uniqKey="Bedding T" first="T. R." last="Bedding">T. R. Bedding</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>Sydney, NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>Sydney, NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Huber, D" sort="Huber, D" uniqKey="Huber D" first="D." last="Huber">D. Huber</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>Sydney, NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Frandsen, S" sort="Frandsen, S" uniqKey="Frandsen S" first="S." last="Frandsen">S. Frandsen</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Karoff, C" sort="Karoff, C" uniqKey="Karoff C" first="C." last="Karoff">C. Karoff</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>10 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Demarque, P" sort="Demarque, P" uniqKey="Demarque P" first="P." last="Demarque">P. Demarque</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Department of Astronomy, Yale University</s1><s2>New Haven, CT 06520-8101</s2><s3>USA</s3><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Fanelli, M N" sort="Fanelli, M N" uniqKey="Fanelli M" first="M. N." last="Fanelli">M. N. Fanelli</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Bay Area Environmental Research Institute, NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Kinemuchi, K" sort="Kinemuchi, K" uniqKey="Kinemuchi K" first="K." last="Kinemuchi">K. Kinemuchi</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Bay Area Environmental Research Institute, NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Mullally, F" sort="Mullally, F" uniqKey="Mullally F" first="F." last="Mullally">F. Mullally</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>SETI Institute, NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>14 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">12-0025843</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 12-0025843 INIST</idno><idno type="RBID">Pascal:12-0025843</idno><idno type="wicri:Area/PascalFrancis/Corpus">001712</idno><idno type="wicri:Area/PascalFrancis/Curation">004797</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">MODELING KEPLER OBSERVATIONS OF SOLAR-LIKE OSCILLATIONS IN THE RED GIANT STAR HD 186355</title><author><name sortKey="Jiang, C" sort="Jiang, C" uniqKey="Jiang C" first="C." last="Jiang">C. Jiang</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Astronomy, Beijing Normal University</s1><s2>Beijing 100875</s2><s3>CHN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>République populaire de Chine</country></affiliation></author><author><name sortKey="Jiang, B W" sort="Jiang, B W" uniqKey="Jiang B" first="B. W." last="Jiang">B. W. Jiang</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Astronomy, Beijing Normal University</s1><s2>Beijing 100875</s2><s3>CHN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>République populaire de Chine</country></affiliation></author><author><name sortKey="Christensen Dalsgaard, J" sort="Christensen Dalsgaard, J" uniqKey="Christensen Dalsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Bedding, T R" sort="Bedding, T R" uniqKey="Bedding T" first="T. R." last="Bedding">T. R. Bedding</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>Sydney, NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>Sydney, NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Huber, D" sort="Huber, D" uniqKey="Huber D" first="D." last="Huber">D. Huber</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>Sydney, NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Frandsen, S" sort="Frandsen, S" uniqKey="Frandsen S" first="S." last="Frandsen">S. Frandsen</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Karoff, C" sort="Karoff, C" uniqKey="Karoff C" first="C." last="Karoff">C. Karoff</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>10 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Demarque, P" sort="Demarque, P" uniqKey="Demarque P" first="P." last="Demarque">P. Demarque</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Department of Astronomy, Yale University</s1><s2>New Haven, CT 06520-8101</s2><s3>USA</s3><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Fanelli, M N" sort="Fanelli, M N" uniqKey="Fanelli M" first="M. N." last="Fanelli">M. N. Fanelli</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Bay Area Environmental Research Institute, NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Kinemuchi, K" sort="Kinemuchi, K" uniqKey="Kinemuchi K" first="K." last="Kinemuchi">K. Kinemuchi</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Bay Area Environmental Research Institute, NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Mullally, F" sort="Mullally, F" uniqKey="Mullally F" first="F." last="Mullally">F. Mullally</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>SETI Institute, NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>14 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author></analytic><series><title level="j" type="main">The Astrophysical journal</title><title level="j" type="abbreviated">Astrophys. j.</title><idno type="ISSN">0004-637X</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">The Astrophysical journal</title><title level="j" type="abbreviated">Astrophys. j.</title><idno type="ISSN">0004-637X</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Data analysis</term><term>Effective temperature</term><term>Giant stars</term><term>Hydrogen burning</term><term>Kepler satellite</term><term>Luminosity</term><term>Modelling</term><term>Models</term><term>Oscillation frequency</term><term>Oscillation modes</term><term>Power spectra</term><term>Red giant stars</term><term>Red stars</term><term>Solar type star</term><term>Stellar evolution</term><term>Time series</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Modélisation</term><term>Etoile rouge</term><term>Géante rouge</term><term>Etoile géante</term><term>Satellite Kepler</term><term>Série temporelle</term><term>Fréquence oscillation</term><term>Spectre puissance</term><term>Mode oscillation</term><term>Evolution stellaire</term><term>Température effective</term><term>Luminosité</term><term>Modèle</term><term>Combustion hydrogène</term><term>Analyse donnée</term><term>Etoile type solaire</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We have analyzed oscillations of the red giant star HD 186355 observed by the NASA Kepler satellite. The data consist of the first five quarters of science operations of Kepler, which cover about 13 months. The high-precision time-series data allow us to accurately extract the oscillation frequencies from the power spectrum. We find that the frequency of the maximum oscillation power, ν<sub>max</sub>, and the mean large frequency separation, Δν, are around 106 and 9.4 μHz, respectively. A regular pattern of radial and non-radial oscillation modes is identified by stacking the power spectra in an echelle diagram. We use the scaling relations of Δν and ν<sub>max</sub> to estimate the preliminary asteroseismic mass, which is confirmed with the modeling result (M = 1.45 ± 0.05 M<sub>◦.</sub>) using the Yale Rotating stellar Evolution Code (YREC7). In addition, we constrain the effective temperature, luminosity, and radius from comparisons between observational constraints and models. A number of mixed l = 1 modes are also detected and taken into account in our model comparisons. We find a mean observational period spacing for these mixed modes of about 58 s, suggesting that this red giant branch star is in the shell hydrogen-burning phase.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-637X</s0></fA01><fA02 i1="01"><s0>ASJOAB</s0></fA02><fA03 i2="1"><s0>Astrophys. j.</s0></fA03><fA05><s2>742</s2></fA05><fA06><s2>2</s2><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>MODELING KEPLER OBSERVATIONS OF SOLAR-LIKE OSCILLATIONS IN THE RED GIANT STAR HD 186355</s1></fA08><fA11 i1="01" i2="1"><s1>JIANG (C.)</s1></fA11><fA11 i1="02" i2="1"><s1>JIANG (B. W.)</s1></fA11><fA11 i1="03" i2="1"><s1>CHRISTENSEN-DALSGAARD (J.)</s1></fA11><fA11 i1="04" i2="1"><s1>BEDDING (T. R.)</s1></fA11><fA11 i1="05" i2="1"><s1>STELLO (D.)</s1></fA11><fA11 i1="06" i2="1"><s1>HUBER (D.)</s1></fA11><fA11 i1="07" i2="1"><s1>FRANDSEN (S.)</s1></fA11><fA11 i1="08" i2="1"><s1>KJELDSEN (H.)</s1></fA11><fA11 i1="09" i2="1"><s1>KAROFF (C.)</s1></fA11><fA11 i1="10" i2="1"><s1>MOSSER (B.)</s1></fA11><fA11 i1="11" i2="1"><s1>DEMARQUE (P.)</s1></fA11><fA11 i1="12" i2="1"><s1>FANELLI (M. N.)</s1></fA11><fA11 i1="13" i2="1"><s1>KINEMUCHI (K.)</s1></fA11><fA11 i1="14" i2="1"><s1>MULLALLY (F.)</s1></fA11><fA14 i1="01"><s1>Department of Astronomy, Beijing Normal University</s1><s2>Beijing 100875</s2><s3>CHN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></fA14><fA14 i1="02"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></fA14><fA14 i1="03"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>Sydney, NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ></fA14><fA14 i1="04"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>10 aut.</sZ></fA14><fA14 i1="05"><s1>Department of Astronomy, Yale University</s1><s2>New Haven, CT 06520-8101</s2><s3>USA</s3><sZ>11 aut.</sZ></fA14><fA14 i1="06"><s1>Bay Area Environmental Research Institute, NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>12 aut.</sZ><sZ>13 aut.</sZ></fA14><fA14 i1="07"><s1>SETI Institute, NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>14 aut.</sZ></fA14><fA20><s2>120.1-120.7</s2></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>512</s2><s5>354000505927740600</s5></fA43><fA44><s0>0000</s0><s1>© 2012 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>12-0025843</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>The Astrophysical journal</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We have analyzed oscillations of the red giant star HD 186355 observed by the NASA Kepler satellite. The data consist of the first five quarters of science operations of Kepler, which cover about 13 months. The high-precision time-series data allow us to accurately extract the oscillation frequencies from the power spectrum. We find that the frequency of the maximum oscillation power, ν<sub>max</sub>, and the mean large frequency separation, Δν, are around 106 and 9.4 μHz, respectively. A regular pattern of radial and non-radial oscillation modes is identified by stacking the power spectra in an echelle diagram. We use the scaling relations of Δν and ν<sub>max</sub> to estimate the preliminary asteroseismic mass, which is confirmed with the modeling result (M = 1.45 ± 0.05 M<sub>◦.</sub>) using the Yale Rotating stellar Evolution Code (YREC7). In addition, we constrain the effective temperature, luminosity, and radius from comparisons between observational constraints and models. A number of mixed l = 1 modes are also detected and taken into account in our model comparisons. We find a mean observational period spacing for these mixed modes of about 58 s, suggesting that this red giant branch star is in the shell hydrogen-burning phase.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Modélisation</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Modelling</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Etoile rouge</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Red stars</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Géante rouge</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Red giant stars</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Etoile géante</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Giant stars</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Satellite Kepler</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Kepler satellite</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Satélite Kepler</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Série temporelle</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Time series</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Fréquence oscillation</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Oscillation frequency</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Frecuencia oscilación</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Spectre puissance</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Power spectra</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Mode oscillation</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Oscillation modes</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Evolution stellaire</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Stellar evolution</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Température effective</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Effective temperature</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Luminosité</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Luminosity</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Modèle</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Models</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Modelo</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Combustion hydrogène</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Hydrogen burning</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Analyse donnée</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Data analysis</s0><s5>40</s5></fC03><fC03 i1="16" i2="X" l="FRE"><s0>Etoile type solaire</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="ENG"><s0>Solar type star</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="SPA"><s0>Estrella tipo solar</s0><s5>41</s5></fC03><fN21><s1>009</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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|wiki= Wicri/Asie
|area= AustralieFrV1
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|texte= MODELING KEPLER OBSERVATIONS OF SOLAR-LIKE OSCILLATIONS IN THE RED GIANT STAR HD 186355
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