ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS
Identifieur interne : 002246 ( PascalFrancis/Corpus ); précédent : 002245; suivant : 002247ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS
Auteurs : D. Huber ; T. R. Bedding ; D. Stello ; B. Mosser ; S. Mathur ; T. Kallinger ; S. Hekker ; Y. P. Elsworth ; D. L. Buzasi ; J. De Ridder ; R. L. Gilliland ; H. Kjeldseni ; W. J. Chaplin ; R. A. Garcia ; S. J. Hale ; H. L. Preston ; T. R. White ; W. J. Borucki ; J. Christensen-Dalsgaard ; B. D. Clarke ; J. M. Jenkins ; D. KochSource :
- The Astrophysical journal [ 0004-637X ] ; 2010.
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Abstract
We have studied solar-like oscillations in ˜800 red giant stars using Kepler long-cadence photometry. The sample includes stars ranging in evolution from the lower part of the red giant branch to the helium main sequence. We investigate the relation between the large frequency separation (Δν) and the frequency of maximum power (νmax) and show that it is different for red giants than for main-sequence stars, which is consistent with evolutionary models and scaling relations. The distributions of νmax and Δν are in qualitative agreement with a simple stellar population model of the Kepler field, including the first evidence for a secondary clump population characterized by M ? 2 M◦. and νmax ≃ 40-110 μHz. We measured the small frequency separations δν02 and δν01 in over 400 stars and δν03 in over 40. We present C-D diagrams for I = 1, 2, and 3 and show that the frequency separation ratios δν02/Δν and δν01/Δν have opposite trends as a function of Δν. The data show a narrowing of the l = 1 ridge toward lower νmax, in agreement with models predicting more efficient mode trapping in stars with higher luminosity. We investigate the offset ∈ in the asymptotic relation and find a clear correlation with Δν, demonstrating that it is related to fundamental stellar parameters. Finally, we present the first amplitude-νmax relation for Kepler red giants. We observe a lack of low-amplitude stars for νmax ? 110 μHz and find that, for a given νmax between 40 and 110 μHz, stars with lower Δν (and consequently higher mass) tend to show lower amplitudes than stars with higher Δν.
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Format Inist (serveur)
| NO : | PASCAL 10-0518684 INIST |
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| ET : | ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS |
| AU : | HUBER (D.); BEDDING (T. R.); STELLO (D.); MOSSER (B.); MATHUR (S.); KALLINGER (T.); HEKKER (S.); ELSWORTH (Y. P.); BUZASI (D. L.); DE RIDDER (J.); GILLILAND (R. L.); KJELDSENI (H.); CHAPLIN (W. J.); GARCIA (R. A.); HALE (S. J.); PRESTON (H. L.); WHITE (T. R.); BORUCKI (W. J.); CHRISTENSEN-DALSGAARD (J.); CLARKE (B. D.); JENKINS (J. M.); KOCH (D.) |
| AF : | Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney/NSW 2006/Australie (1 aut., 2 aut., 3 aut., 17 aut.); LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris/92195 Meudon/France (4 aut.); High Altitude Observatory, NCAR, P.O. BOX 3000/Boulder, CO 80307/Etats-Unis (5 aut.); Department of Physics and Astronomy, University of British Columbia/Vancouver, BC/Canada (6 aut.); Institute for Astronomy (IFA), University of Vienna/1180 Vienna/Autriche (6 aut.); School of Physics and Astronomy, University of Birmingham, Edgbaston/Birmingham B15 2TT/Royaume-Uni (7 aut., 8 aut., 13 aut., 15 aut.); Eureka Scientific, 2452 Delmer Street Suite 100/Oakland, CA 94602-3017/Etats-Unis (9 aut., 16 aut.); Instituut voor Sterrenkunde, K.U. Leuven/Belgique (10 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (11 aut.); Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University/8000 Aarhus/Danemark (12 aut., 19 aut.); Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay/91191, Gif-sur-Yvette/France (14 aut.); Department of Mathematical Sciences, University of South Africa, Box 392 UNISA 0003/Afrique du Sud (16 aut.); NASA Ames Research Center, MS 244-30/Moffett Field, CA 94035/Etats-Unis (18 aut., 22 aut.); SETI Institute, NASA Ames Research Center, MS 244-30/Moffett Field, CA 94035/Etats-Unis (20 aut., 21 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2010; Vol. 723; No. 2 p. 1; Pp. 1607-1617; Bibl. 3/4 p. |
| LA : | Anglais |
| EA : | We have studied solar-like oscillations in ˜800 red giant stars using Kepler long-cadence photometry. The sample includes stars ranging in evolution from the lower part of the red giant branch to the helium main sequence. We investigate the relation between the large frequency separation (Δν) and the frequency of maximum power (νmax) and show that it is different for red giants than for main-sequence stars, which is consistent with evolutionary models and scaling relations. The distributions of νmax and Δν are in qualitative agreement with a simple stellar population model of the Kepler field, including the first evidence for a secondary clump population characterized by M ? 2 M◦. and νmax ≃ 40-110 μHz. We measured the small frequency separations δν02 and δν01 in over 400 stars and δν03 in over 40. We present C-D diagrams for I = 1, 2, and 3 and show that the frequency separation ratios δν02/Δν and δν01/Δν have opposite trends as a function of Δν. The data show a narrowing of the l = 1 ridge toward lower νmax, in agreement with models predicting more efficient mode trapping in stars with higher luminosity. We investigate the offset ∈ in the asymptotic relation and find a clear correlation with Δν, demonstrating that it is related to fundamental stellar parameters. Finally, we present the first amplitude-νmax relation for Kepler red giants. We observe a lack of low-amplitude stars for νmax ? 110 μHz and find that, for a given νmax between 40 and 110 μHz, stars with lower Δν (and consequently higher mass) tend to show lower amplitudes than stars with higher Δν. |
| CC : | 001E03 |
| FD : | Astéroséismologie; Géante rouge; Etoile rouge; Etoile géante; Photométrie; Evolution stellaire; Etoile séquence principale; Modèle stellaire; Population stellaire; Fonction tendance; Luminosité; Corrélation; Paramètre physique; Etoile type avancé |
| ED : | Astroseismology; Red giant stars; Red stars; Giant stars; Photometry; Stellar evolution; Main sequence stars; Star models; Stellar population; Trend function; Luminosity; Correlations; Physical parameter; Late type stars |
| SD : | Población estelar; Función tendencia; Parámetro físico |
| LO : | INIST-512.354000191409130520 |
| ID : | 10-0518684 |
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Elsworth</name><affiliation><inist:fA14 i1="06"><s1>School of Physics and Astronomy, University of Birmingham, Edgbaston</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Buzasi, D L" sort="Buzasi, D L" uniqKey="Buzasi D" first="D. L." last="Buzasi">D. L. Buzasi</name><affiliation><inist:fA14 i1="07"><s1>Eureka Scientific, 2452 Delmer Street Suite 100</s1><s2>Oakland, CA 94602-3017</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></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><inist:fA14 i1="08"><s1>Instituut voor Sterrenkunde, K.U. Leuven</s1><s3>BEL</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilliland, R L" sort="Gilliland, R L" uniqKey="Gilliland R" first="R. L." last="Gilliland">R. L. Gilliland</name><affiliation><inist:fA14 i1="09"><s1>Space Telescope Science Institute, 3700 San Martin Drive</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kjeldseni, H" sort="Kjeldseni, H" uniqKey="Kjeldseni H" first="H." last="Kjeldseni">H. Kjeldseni</name><affiliation><inist:fA14 i1="10"><s1>Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>12 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Chaplin, W J" sort="Chaplin, W J" uniqKey="Chaplin W" first="W. J." last="Chaplin">W. J. Chaplin</name><affiliation><inist:fA14 i1="06"><s1>School of Physics and Astronomy, University of Birmingham, Edgbaston</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Garcia, R A" sort="Garcia, R A" uniqKey="Garcia R" first="R. A." last="Garcia">R. A. Garcia</name><affiliation><inist:fA14 i1="11"><s1>Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay</s1><s2>91191, Gif-sur-Yvette</s2><s3>FRA</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Hale, S J" sort="Hale, S J" uniqKey="Hale S" first="S. J." last="Hale">S. J. Hale</name><affiliation><inist:fA14 i1="06"><s1>School of Physics and Astronomy, University of Birmingham, Edgbaston</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Preston, H L" sort="Preston, H L" uniqKey="Preston H" first="H. L." last="Preston">H. L. Preston</name><affiliation><inist:fA14 i1="07"><s1>Eureka Scientific, 2452 Delmer Street Suite 100</s1><s2>Oakland, CA 94602-3017</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="12"><s1>Department of Mathematical Sciences, University of South Africa, Box 392 UNISA 0003</s1><s3>ZAF</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="White, T R" sort="White, T R" uniqKey="White T" first="T. R." last="White">T. R. White</name><affiliation><inist:fA14 i1="01"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Borucki, W J" sort="Borucki, W J" uniqKey="Borucki W" first="W. J." last="Borucki">W. J. Borucki</name><affiliation><inist:fA14 i1="13"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></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><inist:fA14 i1="10"><s1>Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>12 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Clarke, B D" sort="Clarke, B D" uniqKey="Clarke B" first="B. D." last="Clarke">B. D. Clarke</name><affiliation><inist:fA14 i1="14"><s1>SETI Institute, NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>20 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jenkins, J M" sort="Jenkins, J M" uniqKey="Jenkins J" first="J. M." last="Jenkins">J. M. Jenkins</name><affiliation><inist:fA14 i1="14"><s1>SETI Institute, NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>20 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Koch, D" sort="Koch, D" uniqKey="Koch D" first="D." last="Koch">D. Koch</name><affiliation><inist:fA14 i1="13"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">10-0518684</idno><date when="2010">2010</date><idno type="stanalyst">PASCAL 10-0518684 INIST</idno><idno type="RBID">Pascal:10-0518684</idno><idno type="wicri:Area/PascalFrancis/Corpus">002246</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS</title><author><name sortKey="Huber, D" sort="Huber, D" uniqKey="Huber D" first="D." last="Huber">D. Huber</name><affiliation><inist:fA14 i1="01"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></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><inist:fA14 i1="01"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Stello, D" sort="Stello, D" uniqKey="Stello D" first="D." last="Stello">D. Stello</name><affiliation><inist:fA14 i1="01"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Mosser, B" sort="Mosser, B" uniqKey="Mosser B" first="B." last="Mosser">B. Mosser</name><affiliation><inist:fA14 i1="02"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Mathur, S" sort="Mathur, S" uniqKey="Mathur S" first="S." last="Mathur">S. Mathur</name><affiliation><inist:fA14 i1="03"><s1>High Altitude Observatory, NCAR, P.O. BOX 3000</s1><s2>Boulder, CO 80307</s2><s3>USA</s3><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kallinger, T" sort="Kallinger, T" uniqKey="Kallinger T" first="T." last="Kallinger">T. Kallinger</name><affiliation><inist:fA14 i1="04"><s1>Department of Physics and Astronomy, University of British Columbia</s1><s2>Vancouver, BC</s2><s3>CAN</s3><sZ>6 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="05"><s1>Institute for Astronomy (IFA), University of Vienna</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name><affiliation><inist:fA14 i1="06"><s1>School of Physics and Astronomy, University of Birmingham, Edgbaston</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Elsworth, Y P" sort="Elsworth, Y P" uniqKey="Elsworth Y" first="Y. P." last="Elsworth">Y. P. Elsworth</name><affiliation><inist:fA14 i1="06"><s1>School of Physics and Astronomy, University of Birmingham, Edgbaston</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Buzasi, D L" sort="Buzasi, D L" uniqKey="Buzasi D" first="D. L." last="Buzasi">D. L. Buzasi</name><affiliation><inist:fA14 i1="07"><s1>Eureka Scientific, 2452 Delmer Street Suite 100</s1><s2>Oakland, CA 94602-3017</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></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><inist:fA14 i1="08"><s1>Instituut voor Sterrenkunde, K.U. Leuven</s1><s3>BEL</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilliland, R L" sort="Gilliland, R L" uniqKey="Gilliland R" first="R. L." last="Gilliland">R. L. Gilliland</name><affiliation><inist:fA14 i1="09"><s1>Space Telescope Science Institute, 3700 San Martin Drive</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kjeldseni, H" sort="Kjeldseni, H" uniqKey="Kjeldseni H" first="H." last="Kjeldseni">H. Kjeldseni</name><affiliation><inist:fA14 i1="10"><s1>Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>12 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Chaplin, W J" sort="Chaplin, W J" uniqKey="Chaplin W" first="W. J." last="Chaplin">W. J. Chaplin</name><affiliation><inist:fA14 i1="06"><s1>School of Physics and Astronomy, University of Birmingham, Edgbaston</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Garcia, R A" sort="Garcia, R A" uniqKey="Garcia R" first="R. A." last="Garcia">R. A. Garcia</name><affiliation><inist:fA14 i1="11"><s1>Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay</s1><s2>91191, Gif-sur-Yvette</s2><s3>FRA</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Hale, S J" sort="Hale, S J" uniqKey="Hale S" first="S. J." last="Hale">S. J. Hale</name><affiliation><inist:fA14 i1="06"><s1>School of Physics and Astronomy, University of Birmingham, Edgbaston</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Preston, H L" sort="Preston, H L" uniqKey="Preston H" first="H. L." last="Preston">H. L. Preston</name><affiliation><inist:fA14 i1="07"><s1>Eureka Scientific, 2452 Delmer Street Suite 100</s1><s2>Oakland, CA 94602-3017</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="12"><s1>Department of Mathematical Sciences, University of South Africa, Box 392 UNISA 0003</s1><s3>ZAF</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="White, T R" sort="White, T R" uniqKey="White T" first="T. R." last="White">T. R. White</name><affiliation><inist:fA14 i1="01"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Borucki, W J" sort="Borucki, W J" uniqKey="Borucki W" first="W. J." last="Borucki">W. J. Borucki</name><affiliation><inist:fA14 i1="13"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></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><inist:fA14 i1="10"><s1>Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>12 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Clarke, B D" sort="Clarke, B D" uniqKey="Clarke B" first="B. D." last="Clarke">B. D. Clarke</name><affiliation><inist:fA14 i1="14"><s1>SETI Institute, NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>20 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jenkins, J M" sort="Jenkins, J M" uniqKey="Jenkins J" first="J. M." last="Jenkins">J. M. Jenkins</name><affiliation><inist:fA14 i1="14"><s1>SETI Institute, NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>20 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Koch, D" sort="Koch, D" uniqKey="Koch D" first="D." last="Koch">D. Koch</name><affiliation><inist:fA14 i1="13"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>18 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></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="2010">2010</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>Astroseismology</term><term>Correlations</term><term>Giant stars</term><term>Late type stars</term><term>Luminosity</term><term>Main sequence stars</term><term>Photometry</term><term>Physical parameter</term><term>Red giant stars</term><term>Red stars</term><term>Star models</term><term>Stellar evolution</term><term>Stellar population</term><term>Trend function</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Astéroséismologie</term><term>Géante rouge</term><term>Etoile rouge</term><term>Etoile géante</term><term>Photométrie</term><term>Evolution stellaire</term><term>Etoile séquence principale</term><term>Modèle stellaire</term><term>Population stellaire</term><term>Fonction tendance</term><term>Luminosité</term><term>Corrélation</term><term>Paramètre physique</term><term>Etoile type avancé</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We have studied solar-like oscillations in ˜800 red giant stars using Kepler long-cadence photometry. The sample includes stars ranging in evolution from the lower part of the red giant branch to the helium main sequence. We investigate the relation between the large frequency separation (Δν) and the frequency of maximum power (ν<sub>max</sub>) and show that it is different for red giants than for main-sequence stars, which is consistent with evolutionary models and scaling relations. The distributions of ν<sub>max</sub> and Δν are in qualitative agreement with a simple stellar population model of the Kepler field, including the first evidence for a secondary clump population characterized by M ? 2 M<sub>◦.</sub> and ν<sub>max</sub> ≃ 40-110 μHz. We measured the small frequency separations δν<sub>02</sub> and δν<sub>01</sub> in over 400 stars and δν<sub>03</sub> in over 40. We present C-D diagrams for I = 1, 2, and 3 and show that the frequency separation ratios δν<sub>02</sub>/Δν and δν<sub>01</sub>/Δν have opposite trends as a function of Δν. The data show a narrowing of the l = 1 ridge toward lower ν<sub>max</sub>, in agreement with models predicting more efficient mode trapping in stars with higher luminosity. We investigate the offset ∈ in the asymptotic relation and find a clear correlation with Δν, demonstrating that it is related to fundamental stellar parameters. Finally, we present the first amplitude-ν<sub>max</sub> relation for Kepler red giants. We observe a lack of low-amplitude stars for ν<sub>max </sub>? 110 μHz and find that, for a given ν<sub>max</sub> between 40 and 110 μHz, stars with lower Δν (and consequently higher mass) tend to show lower amplitudes than stars with higher Δν.</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>723</s2></fA05><fA06><s2>2</s2><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS</s1></fA08><fA11 i1="01" i2="1"><s1>HUBER (D.)</s1></fA11><fA11 i1="02" i2="1"><s1>BEDDING (T. R.)</s1></fA11><fA11 i1="03" i2="1"><s1>STELLO (D.)</s1></fA11><fA11 i1="04" i2="1"><s1>MOSSER (B.)</s1></fA11><fA11 i1="05" i2="1"><s1>MATHUR (S.)</s1></fA11><fA11 i1="06" i2="1"><s1>KALLINGER (T.)</s1></fA11><fA11 i1="07" i2="1"><s1>HEKKER (S.)</s1></fA11><fA11 i1="08" i2="1"><s1>ELSWORTH (Y. P.)</s1></fA11><fA11 i1="09" i2="1"><s1>BUZASI (D. L.)</s1></fA11><fA11 i1="10" i2="1"><s1>DE RIDDER (J.)</s1></fA11><fA11 i1="11" i2="1"><s1>GILLILAND (R. L.)</s1></fA11><fA11 i1="12" i2="1"><s1>KJELDSENI (H.)</s1></fA11><fA11 i1="13" i2="1"><s1>CHAPLIN (W. J.)</s1></fA11><fA11 i1="14" i2="1"><s1>GARCIA (R. A.)</s1></fA11><fA11 i1="15" i2="1"><s1>HALE (S. J.)</s1></fA11><fA11 i1="16" i2="1"><s1>PRESTON (H. L.)</s1></fA11><fA11 i1="17" i2="1"><s1>WHITE (T. R.)</s1></fA11><fA11 i1="18" i2="1"><s1>BORUCKI (W. J.)</s1></fA11><fA11 i1="19" i2="1"><s1>CHRISTENSEN-DALSGAARD (J.)</s1></fA11><fA11 i1="20" i2="1"><s1>CLARKE (B. D.)</s1></fA11><fA11 i1="21" i2="1"><s1>JENKINS (J. M.)</s1></fA11><fA11 i1="22" i2="1"><s1>KOCH (D.)</s1></fA11><fA14 i1="01"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>17 aut.</sZ></fA14><fA14 i1="02"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>4 aut.</sZ></fA14><fA14 i1="03"><s1>High Altitude Observatory, NCAR, P.O. BOX 3000</s1><s2>Boulder, CO 80307</s2><s3>USA</s3><sZ>5 aut.</sZ></fA14><fA14 i1="04"><s1>Department of Physics and Astronomy, University of British Columbia</s1><s2>Vancouver, BC</s2><s3>CAN</s3><sZ>6 aut.</sZ></fA14><fA14 i1="05"><s1>Institute for Astronomy (IFA), University of Vienna</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>6 aut.</sZ></fA14><fA14 i1="06"><s1>School of Physics and Astronomy, University of Birmingham, Edgbaston</s1><s2>Birmingham B15 2TT</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="07"><s1>Eureka Scientific, 2452 Delmer Street Suite 100</s1><s2>Oakland, CA 94602-3017</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>16 aut.</sZ></fA14><fA14 i1="08"><s1>Instituut voor Sterrenkunde, K.U. Leuven</s1><s3>BEL</s3><sZ>10 aut.</sZ></fA14><fA14 i1="09"><s1>Space Telescope Science Institute, 3700 San Martin Drive</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>11 aut.</sZ></fA14><fA14 i1="10"><s1>Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>12 aut.</sZ><sZ>19 aut.</sZ></fA14><fA14 i1="11"><s1>Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay</s1><s2>91191, Gif-sur-Yvette</s2><s3>FRA</s3><sZ>14 aut.</sZ></fA14><fA14 i1="12"><s1>Department of Mathematical Sciences, University of South Africa, Box 392 UNISA 0003</s1><s3>ZAF</s3><sZ>16 aut.</sZ></fA14><fA14 i1="13"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>18 aut.</sZ><sZ>22 aut.</sZ></fA14><fA14 i1="14"><s1>SETI Institute, NASA Ames Research Center, MS 244-30</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>20 aut.</sZ><sZ>21 aut.</sZ></fA14><fA20><s1>1607-1617</s1></fA20><fA21><s1>2010</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>512</s2><s5>354000191409130520</s5></fA43><fA44><s0>0000</s0><s1>© 2010 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>10-0518684</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 studied solar-like oscillations in ˜800 red giant stars using Kepler long-cadence photometry. The sample includes stars ranging in evolution from the lower part of the red giant branch to the helium main sequence. We investigate the relation between the large frequency separation (Δν) and the frequency of maximum power (ν<sub>max</sub>) and show that it is different for red giants than for main-sequence stars, which is consistent with evolutionary models and scaling relations. The distributions of ν<sub>max</sub> and Δν are in qualitative agreement with a simple stellar population model of the Kepler field, including the first evidence for a secondary clump population characterized by M ? 2 M<sub>◦.</sub> and ν<sub>max</sub> ≃ 40-110 μHz. We measured the small frequency separations δν<sub>02</sub> and δν<sub>01</sub> in over 400 stars and δν<sub>03</sub> in over 40. We present C-D diagrams for I = 1, 2, and 3 and show that the frequency separation ratios δν<sub>02</sub>/Δν and δν<sub>01</sub>/Δν have opposite trends as a function of Δν. The data show a narrowing of the l = 1 ridge toward lower ν<sub>max</sub>, in agreement with models predicting more efficient mode trapping in stars with higher luminosity. We investigate the offset ∈ in the asymptotic relation and find a clear correlation with Δν, demonstrating that it is related to fundamental stellar parameters. Finally, we present the first amplitude-ν<sub>max</sub> relation for Kepler red giants. We observe a lack of low-amplitude stars for ν<sub>max </sub>? 110 μHz and find that, for a given ν<sub>max</sub> between 40 and 110 μHz, stars with lower Δν (and consequently higher mass) tend to show lower amplitudes than stars with higher Δν.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Astéroséismologie</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Astroseismology</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Géante rouge</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Red giant stars</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Etoile rouge</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Red 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="3" l="FRE"><s0>Photométrie</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Photometry</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Evolution stellaire</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Stellar evolution</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Etoile séquence principale</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Main sequence stars</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Modèle stellaire</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Star models</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Population stellaire</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Stellar population</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Población estelar</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Fonction tendance</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Trend function</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Función tendencia</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Luminosité</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Luminosity</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Corrélation</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Correlations</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Paramètre physique</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Physical parameter</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Parámetro físico</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Etoile type avancé</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Late type stars</s0><s5>39</s5></fC03><fN21><s1>347</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 10-0518684 INIST</NO><ET>ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS</ET><AU>HUBER (D.); BEDDING (T. R.); STELLO (D.); MOSSER (B.); MATHUR (S.); KALLINGER (T.); HEKKER (S.); ELSWORTH (Y. P.); BUZASI (D. L.); DE RIDDER (J.); GILLILAND (R. L.); KJELDSENI (H.); CHAPLIN (W. J.); GARCIA (R. A.); HALE (S. J.); PRESTON (H. L.); WHITE (T. R.); BORUCKI (W. J.); CHRISTENSEN-DALSGAARD (J.); CLARKE (B. D.); JENKINS (J. M.); KOCH (D.)</AU><AF>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney/NSW 2006/Australie (1 aut., 2 aut., 3 aut., 17 aut.); LESIA, CNRS, Université Pierre et Marie Curie, Université Denis, Diderot, Observatoire de Paris/92195 Meudon/France (4 aut.); High Altitude Observatory, NCAR, P.O. BOX 3000/Boulder, CO 80307/Etats-Unis (5 aut.); Department of Physics and Astronomy, University of British Columbia/Vancouver, BC/Canada (6 aut.); Institute for Astronomy (IFA), University of Vienna/1180 Vienna/Autriche (6 aut.); School of Physics and Astronomy, University of Birmingham, Edgbaston/Birmingham B15 2TT/Royaume-Uni (7 aut., 8 aut., 13 aut., 15 aut.); Eureka Scientific, 2452 Delmer Street Suite 100/Oakland, CA 94602-3017/Etats-Unis (9 aut., 16 aut.); Instituut voor Sterrenkunde, K.U. Leuven/Belgique (10 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (11 aut.); Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University/8000 Aarhus/Danemark (12 aut., 19 aut.); Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay/91191, Gif-sur-Yvette/France (14 aut.); Department of Mathematical Sciences, University of South Africa, Box 392 UNISA 0003/Afrique du Sud (16 aut.); NASA Ames Research Center, MS 244-30/Moffett Field, CA 94035/Etats-Unis (18 aut., 22 aut.); SETI Institute, NASA Ames Research Center, MS 244-30/Moffett Field, CA 94035/Etats-Unis (20 aut., 21 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2010; Vol. 723; No. 2 p. 1; Pp. 1607-1617; Bibl. 3/4 p.</SO><LA>Anglais</LA><EA>We have studied solar-like oscillations in ˜800 red giant stars using Kepler long-cadence photometry. The sample includes stars ranging in evolution from the lower part of the red giant branch to the helium main sequence. We investigate the relation between the large frequency separation (Δν) and the frequency of maximum power (ν<sub>max</sub>) and show that it is different for red giants than for main-sequence stars, which is consistent with evolutionary models and scaling relations. The distributions of ν<sub>max</sub> and Δν are in qualitative agreement with a simple stellar population model of the Kepler field, including the first evidence for a secondary clump population characterized by M ? 2 M<sub>◦.</sub> and ν<sub>max</sub> ≃ 40-110 μHz. We measured the small frequency separations δν<sub>02</sub> and δν<sub>01</sub> in over 400 stars and δν<sub>03</sub> in over 40. We present C-D diagrams for I = 1, 2, and 3 and show that the frequency separation ratios δν<sub>02</sub>/Δν and δν<sub>01</sub>/Δν have opposite trends as a function of Δν. The data show a narrowing of the l = 1 ridge toward lower ν<sub>max</sub>, in agreement with models predicting more efficient mode trapping in stars with higher luminosity. We investigate the offset ∈ in the asymptotic relation and find a clear correlation with Δν, demonstrating that it is related to fundamental stellar parameters. Finally, we present the first amplitude-ν<sub>max</sub> relation for Kepler red giants. We observe a lack of low-amplitude stars for ν<sub>max </sub>? 110 μHz and find that, for a given ν<sub>max</sub> between 40 and 110 μHz, stars with lower Δν (and consequently higher mass) tend to show lower amplitudes than stars with higher Δν.</EA><CC>001E03</CC><FD>Astéroséismologie; Géante rouge; Etoile rouge; Etoile géante; Photométrie; Evolution stellaire; Etoile séquence principale; Modèle stellaire; Population stellaire; Fonction tendance; Luminosité; Corrélation; Paramètre physique; Etoile type avancé</FD><ED>Astroseismology; Red giant stars; Red stars; Giant stars; Photometry; Stellar evolution; Main sequence stars; Star models; Stellar population; Trend function; Luminosity; Correlations; Physical parameter; Late type stars</ED><SD>Población estelar; Función tendencia; Parámetro físico</SD><LO>INIST-512.354000191409130520</LO><ID>10-0518684</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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