Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819
Identifieur interne : 004842 ( PascalFrancis/Curation ); précédent : 004841; suivant : 004843Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819
Auteurs : A. Miglio [Royaume-Uni] ; K. Brogaard [Canada] ; D. Stello [Australie] ; W. J. Chaplin [Royaume-Uni] ; F. D' Antona [Italie] ; J. Montalban [Belgique] ; S. Basu [États-Unis] ; A. Bressan [Italie] ; F. Grundahl [Danemark] ; M. Pinsonneault [États-Unis] ; A. M. Serenelli [Espagne] ; Y. Elsworth [Royaume-Uni] ; S. Hekker [Royaume-Uni, Pays-Bas] ; T. Kallinger [Canada] ; B. Mosser [France] ; P. Ventura [Italie] ; A. Bonanno [Italie] ; A. Noels [Belgique] ; V. Silva Aguirre [Allemagne] ; R. Szabo [Hongrie] ; J. Li [États-Unis] ; S. Mccauliff [États-Unis] ; C. K. Middour [États-Unis] ; H. Kjeldsen [Danemark]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2012.
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Abstract
Mass-loss of red giant branch (RGB) stars is still poorly determined, despite its crucial role in the chemical enrichment of galaxies. Thanks to the recent detection of solar-like oscillations in G-K giants in open clusters with Kepler, we can now directly determine stellar masses for a statistically significant sample of stars in the old open clusters NGC 6791 and 6819. The aim of this work is to constrain the integrated RGB mass-loss by comparing the average mass of stars in the red clump (RC) with that of stars in the low-luminosity portion of the RGB [i.e. stars with L ? L(RC)]. Stellar masses were determined by combining the available seismic parameters vmax and Δv with additional photometric constraints and with independent distance estimates. We measured the masses of 40 stars on the RGB and 19 in the RC of the old metal-rich cluster NGC 6791. We find that the difference between the average mass of RGB and RC stars is small, but significant [ΔM? = 0.09 ± 0.03 (random) ±0.04 (systematic) M◦.]. Interestingly, such a small ΔM? does not support scenarios of an extreme mass-loss for this metal-rich cluster. If we describe the mass-loss rate with Reimers prescription, a first comparison with isochrones suggests that the observed AM? is compatible with a mass-loss efficiency parameter in the range 0.1 ? η ? 0.3. Less stringent constraints on the RGB mass-loss rate are set by the analysis of the ˜2 Gyr old NGC 6819, largely due to the lower mass-loss expected for this cluster, and to the lack of an independent and accurate distance determination. In the near future, additional constraints from frequencies of individual pulsation modes and spectroscopic effective temperatures will allow further stringent tests of the Δv and vmax scaling relations, which provide a novel, and potentially very accurate, means of determining stellar radii and masses.
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<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819</title><author><name sortKey="Miglio, A" sort="Miglio, A" uniqKey="Miglio A" first="A." last="Miglio">A. Miglio</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics and Astronomy, University of Birmingham</s1><s2>Edgbaston, Birmingham B15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Brogaard, K" sort="Brogaard, K" uniqKey="Brogaard K" first="K." last="Brogaard">K. Brogaard</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, University of Victoria, PO Box 3055</s1><s2>Victoria, BC V8W 3P6</s2><s3>CAN</s3><sZ>2 aut.</sZ></inist:fA14><country>Canada</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>NSW 2006</s2><s3>AUS</s3><sZ>3 aut.</sZ></inist:fA14><country>Australie</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics and Astronomy, University of Birmingham</s1><s2>Edgbaston, Birmingham B15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Antona, F D" sort="Antona, F D" uniqKey="Antona F" first="F. D'" last="Antona">F. D' Antona</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>INAF - Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio Catone (RM</s1><s3>ITA</s3><sZ>5 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Montalban, J" sort="Montalban, J" uniqKey="Montalban J" first="J." last="Montalban">J. Montalban</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Institut d'Astrophysique et de Géophysique de l'Université de Liège, Allée du 6 Août, 17</s1><s2>4000 Liège</s2><s3>BEL</s3><sZ>6 aut.</sZ><sZ>18 aut.</sZ></inist:fA14><country>Belgique</country></affiliation></author><author><name sortKey="Basu, S" sort="Basu, S" uniqKey="Basu S" first="S." last="Basu">S. Basu</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Department of Astronomy, Yale University, PO Box 208101</s1><s2>New Haven, CT 06520-8101</s2><s3>USA</s3><sZ>7 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Bressan, A" sort="Bressan, A" uniqKey="Bressan A" first="A." last="Bressan">A. Bressan</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>SISSA, via Bonomea 265</s1><s2>34136 Trieste</s2><s3>ITA</s3><sZ>8 aut.</sZ></inist:fA14><country>Italie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>8 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Grundahl, F" sort="Grundahl, F" uniqKey="Grundahl F" first="F." last="Grundahl">F. Grundahl</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, Building 1520, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>9 aut.</sZ><sZ>24 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Pinsonneault, M" sort="Pinsonneault, M" uniqKey="Pinsonneault M" first="M." last="Pinsonneault">M. Pinsonneault</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Department of Astronomy, Ohio State University, 140 West 18th Avenue</s1><s2>Columbus, OH 43210</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Serenelli, A M" sort="Serenelli, A M" uniqKey="Serenelli A" first="A. M." last="Serenelli">A. M. Serenelli</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>Institute for Space Sciences (CSIC-IEEC), Facultad de Ciencies, Campus UAB</s1><s2>08193 Bellaterra</s2><s3>ESP</s3><sZ>11 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Elsworth, Y" sort="Elsworth, Y" uniqKey="Elsworth Y" first="Y." last="Elsworth">Y. Elsworth</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics and Astronomy, University of Birmingham</s1><s2>Edgbaston, Birmingham B15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics and Astronomy, University of Birmingham</s1><s2>Edgbaston, Birmingham B15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904</s1><s2>1098 XH Amsterdam</s2><s3>NLD</s3><sZ>13 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Kallinger, T" sort="Kallinger, T" uniqKey="Kallinger T" first="T." last="Kallinger">T. Kallinger</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Department of Physics and Astronomy, University of British Colombia, 6224 Agricultural Road</s1><s2>Vancouver, BC V6T 1Z1</s2><s3>CAN</s3><sZ>14 aut.</sZ></inist:fA14><country>Canada</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="14"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>15 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Ventura, P" sort="Ventura, P" uniqKey="Ventura P" first="P." last="Ventura">P. Ventura</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>INAF - Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio Catone (RM</s1><s3>ITA</s3><sZ>5 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Bonanno, A" sort="Bonanno, A" uniqKey="Bonanno A" first="A." last="Bonanno">A. Bonanno</name><affiliation wicri:level="1"><inist:fA14 i1="15"><s1>INAF - Osservatorio Astrofisico di Catania, Via S.Sofia 78</s1><s2>95123 Catania</s2><s3>ITA</s3><sZ>17 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Noels, A" sort="Noels, A" uniqKey="Noels A" first="A." last="Noels">A. Noels</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Institut d'Astrophysique et de Géophysique de l'Université de Liège, Allée du 6 Août, 17</s1><s2>4000 Liège</s2><s3>BEL</s3><sZ>6 aut.</sZ><sZ>18 aut.</sZ></inist:fA14><country>Belgique</country></affiliation></author><author><name sortKey="Silva Aguirre, V" sort="Silva Aguirre, V" uniqKey="Silva Aguirre V" first="V." last="Silva Aguirre">V. Silva Aguirre</name><affiliation wicri:level="1"><inist:fA14 i1="16"><s1>Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>19 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Szabo, R" sort="Szabo, R" uniqKey="Szabo R" first="R." last="Szabo">R. Szabo</name><affiliation wicri:level="1"><inist:fA14 i1="17"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Konkoly Thege Miklos út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>20 aut.</sZ></inist:fA14><country>Hongrie</country></affiliation></author><author><name sortKey="Li, J" sort="Li, J" uniqKey="Li J" first="J." last="Li">J. Li</name><affiliation wicri:level="1"><inist:fA14 i1="18"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>21 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Mccauliff, S" sort="Mccauliff, S" uniqKey="Mccauliff S" first="S." last="Mccauliff">S. Mccauliff</name><affiliation wicri:level="1"><inist:fA14 i1="19"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>22 aut.</sZ><sZ>23 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Middour, C K" sort="Middour, C K" uniqKey="Middour C" first="C. K." last="Middour">C. K. Middour</name><affiliation wicri:level="1"><inist:fA14 i1="19"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>22 aut.</sZ><sZ>23 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, Building 1520, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>9 aut.</sZ><sZ>24 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">12-0049842</idno><date when="2012">2012</date><idno type="stanalyst">PASCAL 12-0049842 INIST</idno><idno type="RBID">Pascal:12-0049842</idno><idno type="wicri:Area/PascalFrancis/Corpus">001668</idno><idno type="wicri:Area/PascalFrancis/Curation">004842</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819</title><author><name sortKey="Miglio, A" sort="Miglio, A" uniqKey="Miglio A" first="A." last="Miglio">A. Miglio</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics and Astronomy, University of Birmingham</s1><s2>Edgbaston, Birmingham B15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Brogaard, K" sort="Brogaard, K" uniqKey="Brogaard K" first="K." last="Brogaard">K. Brogaard</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, University of Victoria, PO Box 3055</s1><s2>Victoria, BC V8W 3P6</s2><s3>CAN</s3><sZ>2 aut.</sZ></inist:fA14><country>Canada</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>NSW 2006</s2><s3>AUS</s3><sZ>3 aut.</sZ></inist:fA14><country>Australie</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics and Astronomy, University of Birmingham</s1><s2>Edgbaston, Birmingham B15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Antona, F D" sort="Antona, F D" uniqKey="Antona F" first="F. D'" last="Antona">F. D' Antona</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>INAF - Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio Catone (RM</s1><s3>ITA</s3><sZ>5 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Montalban, J" sort="Montalban, J" uniqKey="Montalban J" first="J." last="Montalban">J. Montalban</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Institut d'Astrophysique et de Géophysique de l'Université de Liège, Allée du 6 Août, 17</s1><s2>4000 Liège</s2><s3>BEL</s3><sZ>6 aut.</sZ><sZ>18 aut.</sZ></inist:fA14><country>Belgique</country></affiliation></author><author><name sortKey="Basu, S" sort="Basu, S" uniqKey="Basu S" first="S." last="Basu">S. Basu</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Department of Astronomy, Yale University, PO Box 208101</s1><s2>New Haven, CT 06520-8101</s2><s3>USA</s3><sZ>7 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Bressan, A" sort="Bressan, A" uniqKey="Bressan A" first="A." last="Bressan">A. Bressan</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>SISSA, via Bonomea 265</s1><s2>34136 Trieste</s2><s3>ITA</s3><sZ>8 aut.</sZ></inist:fA14><country>Italie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>8 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Grundahl, F" sort="Grundahl, F" uniqKey="Grundahl F" first="F." last="Grundahl">F. Grundahl</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, Building 1520, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>9 aut.</sZ><sZ>24 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author><author><name sortKey="Pinsonneault, M" sort="Pinsonneault, M" uniqKey="Pinsonneault M" first="M." last="Pinsonneault">M. Pinsonneault</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Department of Astronomy, Ohio State University, 140 West 18th Avenue</s1><s2>Columbus, OH 43210</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Serenelli, A M" sort="Serenelli, A M" uniqKey="Serenelli A" first="A. M." last="Serenelli">A. M. Serenelli</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>Institute for Space Sciences (CSIC-IEEC), Facultad de Ciencies, Campus UAB</s1><s2>08193 Bellaterra</s2><s3>ESP</s3><sZ>11 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Elsworth, Y" sort="Elsworth, Y" uniqKey="Elsworth Y" first="Y." last="Elsworth">Y. Elsworth</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics and Astronomy, University of Birmingham</s1><s2>Edgbaston, Birmingham B15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Hekker, S" sort="Hekker, S" uniqKey="Hekker S" first="S." last="Hekker">S. Hekker</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics and Astronomy, University of Birmingham</s1><s2>Edgbaston, Birmingham B15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904</s1><s2>1098 XH Amsterdam</s2><s3>NLD</s3><sZ>13 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Kallinger, T" sort="Kallinger, T" uniqKey="Kallinger T" first="T." last="Kallinger">T. Kallinger</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Department of Physics and Astronomy, University of British Colombia, 6224 Agricultural Road</s1><s2>Vancouver, BC V6T 1Z1</s2><s3>CAN</s3><sZ>14 aut.</sZ></inist:fA14><country>Canada</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="14"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>15 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Ventura, P" sort="Ventura, P" uniqKey="Ventura P" first="P." last="Ventura">P. Ventura</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>INAF - Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio Catone (RM</s1><s3>ITA</s3><sZ>5 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Bonanno, A" sort="Bonanno, A" uniqKey="Bonanno A" first="A." last="Bonanno">A. Bonanno</name><affiliation wicri:level="1"><inist:fA14 i1="15"><s1>INAF - Osservatorio Astrofisico di Catania, Via S.Sofia 78</s1><s2>95123 Catania</s2><s3>ITA</s3><sZ>17 aut.</sZ></inist:fA14><country>Italie</country></affiliation></author><author><name sortKey="Noels, A" sort="Noels, A" uniqKey="Noels A" first="A." last="Noels">A. Noels</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Institut d'Astrophysique et de Géophysique de l'Université de Liège, Allée du 6 Août, 17</s1><s2>4000 Liège</s2><s3>BEL</s3><sZ>6 aut.</sZ><sZ>18 aut.</sZ></inist:fA14><country>Belgique</country></affiliation></author><author><name sortKey="Silva Aguirre, V" sort="Silva Aguirre, V" uniqKey="Silva Aguirre V" first="V." last="Silva Aguirre">V. Silva Aguirre</name><affiliation wicri:level="1"><inist:fA14 i1="16"><s1>Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>19 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Szabo, R" sort="Szabo, R" uniqKey="Szabo R" first="R." last="Szabo">R. Szabo</name><affiliation wicri:level="1"><inist:fA14 i1="17"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Konkoly Thege Miklos út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>20 aut.</sZ></inist:fA14><country>Hongrie</country></affiliation></author><author><name sortKey="Li, J" sort="Li, J" uniqKey="Li J" first="J." last="Li">J. Li</name><affiliation wicri:level="1"><inist:fA14 i1="18"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>21 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Mccauliff, S" sort="Mccauliff, S" uniqKey="Mccauliff S" first="S." last="Mccauliff">S. Mccauliff</name><affiliation wicri:level="1"><inist:fA14 i1="19"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>22 aut.</sZ><sZ>23 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Middour, C K" sort="Middour, C K" uniqKey="Middour C" first="C. K." last="Middour">C. K. Middour</name><affiliation wicri:level="1"><inist:fA14 i1="19"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>22 aut.</sZ><sZ>23 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, Building 1520, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>9 aut.</sZ><sZ>24 aut.</sZ></inist:fA14><country>Danemark</country></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2012">2012</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Astroseismology</term><term>Chemical enrichment</term><term>Distance measurement</term><term>Effective temperature</term><term>Galaxies</term><term>Giant stars</term><term>Isochrone</term><term>Late type stars</term><term>Loss rate</term><term>Luminosity</term><term>Mass loss</term><term>Open clusters</term><term>Red giant stars</term><term>Star clusters</term><term>Stellar mass</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Astéroséismologie</term><term>Amas ouvert</term><term>Géante rouge</term><term>Perte masse</term><term>Etoile géante</term><term>Enrichissement chimique</term><term>Galaxies</term><term>Masse stellaire</term><term>Luminosité</term><term>Taux perte</term><term>Isochrone</term><term>Mesure distance</term><term>Température effective</term><term>Etoile type avancé</term><term>Amas stellaire</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Mass-loss of red giant branch (RGB) stars is still poorly determined, despite its crucial role in the chemical enrichment of galaxies. Thanks to the recent detection of solar-like oscillations in G-K giants in open clusters with Kepler, we can now directly determine stellar masses for a statistically significant sample of stars in the old open clusters NGC 6791 and 6819. The aim of this work is to constrain the integrated RGB mass-loss by comparing the average mass of stars in the red clump (RC) with that of stars in the low-luminosity portion of the RGB [i.e. stars with L ? L(RC)]. Stellar masses were determined by combining the available seismic parameters v<sub>max</sub> and Δv with additional photometric constraints and with independent distance estimates. We measured the masses of 40 stars on the RGB and 19 in the RC of the old metal-rich cluster NGC 6791. We find that the difference between the average mass of RGB and RC stars is small, but significant [ΔM? = 0.09 ± 0.03 (random) ±0.04 (systematic) M<sub>◦.</sub>]. Interestingly, such a small ΔM? does not support scenarios of an extreme mass-loss for this metal-rich cluster. If we describe the mass-loss rate with Reimers prescription, a first comparison with isochrones suggests that the observed AM? is compatible with a mass-loss efficiency parameter in the range 0.1 ? η ? 0.3. Less stringent constraints on the RGB mass-loss rate are set by the analysis of the ˜2 Gyr old NGC 6819, largely due to the lower mass-loss expected for this cluster, and to the lack of an independent and accurate distance determination. In the near future, additional constraints from frequencies of individual pulsation modes and spectroscopic effective temperatures will allow further stringent tests of the Δv and v<sub>max</sub> scaling relations, which provide a novel, and potentially very accurate, means of determining stellar radii and masses.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>419</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819</s1></fA08><fA11 i1="01" i2="1"><s1>MIGLIO (A.)</s1></fA11><fA11 i1="02" i2="1"><s1>BROGAARD (K.)</s1></fA11><fA11 i1="03" i2="1"><s1>STELLO (D.)</s1></fA11><fA11 i1="04" i2="1"><s1>CHAPLIN (W. J.)</s1></fA11><fA11 i1="05" i2="1"><s1>ANTONA (F. D')</s1></fA11><fA11 i1="06" i2="1"><s1>MONTALBAN (J.)</s1></fA11><fA11 i1="07" i2="1"><s1>BASU (S.)</s1></fA11><fA11 i1="08" i2="1"><s1>BRESSAN (A.)</s1></fA11><fA11 i1="09" i2="1"><s1>GRUNDAHL (F.)</s1></fA11><fA11 i1="10" i2="1"><s1>PINSONNEAULT (M.)</s1></fA11><fA11 i1="11" i2="1"><s1>SERENELLI (A. M.)</s1></fA11><fA11 i1="12" i2="1"><s1>ELSWORTH (Y.)</s1></fA11><fA11 i1="13" i2="1"><s1>HEKKER (S.)</s1></fA11><fA11 i1="14" i2="1"><s1>KALLINGER (T.)</s1></fA11><fA11 i1="15" i2="1"><s1>MOSSER (B.)</s1></fA11><fA11 i1="16" i2="1"><s1>VENTURA (P.)</s1></fA11><fA11 i1="17" i2="1"><s1>BONANNO (A.)</s1></fA11><fA11 i1="18" i2="1"><s1>NOELS (A.)</s1></fA11><fA11 i1="19" i2="1"><s1>SILVA AGUIRRE (V.)</s1></fA11><fA11 i1="20" i2="1"><s1>SZABO (R.)</s1></fA11><fA11 i1="21" i2="1"><s1>LI (J.)</s1></fA11><fA11 i1="22" i2="1"><s1>MCCAULIFF (S.)</s1></fA11><fA11 i1="23" i2="1"><s1>MIDDOUR (C. K.)</s1></fA11><fA11 i1="24" i2="1"><s1>KJELDSEN (H.)</s1></fA11><fA14 i1="01"><s1>School of Physics and Astronomy, University of Birmingham</s1><s2>Edgbaston, Birmingham B15 2TT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>4 aut.</sZ><sZ>12 aut.</sZ><sZ>13 aut.</sZ></fA14><fA14 i1="02"><s1>Department of Physics and Astronomy, University of Victoria, PO Box 3055</s1><s2>Victoria, BC V8W 3P6</s2><s3>CAN</s3><sZ>2 aut.</sZ></fA14><fA14 i1="03"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>INAF - Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio Catone (RM</s1><s3>ITA</s3><sZ>5 aut.</sZ><sZ>16 aut.</sZ></fA14><fA14 i1="05"><s1>Institut d'Astrophysique et de Géophysique de l'Université de Liège, Allée du 6 Août, 17</s1><s2>4000 Liège</s2><s3>BEL</s3><sZ>6 aut.</sZ><sZ>18 aut.</sZ></fA14><fA14 i1="06"><s1>Department of Astronomy, Yale University, PO Box 208101</s1><s2>New Haven, CT 06520-8101</s2><s3>USA</s3><sZ>7 aut.</sZ></fA14><fA14 i1="07"><s1>SISSA, via Bonomea 265</s1><s2>34136 Trieste</s2><s3>ITA</s3><sZ>8 aut.</sZ></fA14><fA14 i1="08"><s1>INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>8 aut.</sZ></fA14><fA14 i1="09"><s1>Department of Physics and Astronomy, Building 1520, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>9 aut.</sZ><sZ>24 aut.</sZ></fA14><fA14 i1="10"><s1>Department of Astronomy, Ohio State University, 140 West 18th Avenue</s1><s2>Columbus, OH 43210</s2><s3>USA</s3><sZ>10 aut.</sZ></fA14><fA14 i1="11"><s1>Institute for Space Sciences (CSIC-IEEC), Facultad de Ciencies, Campus UAB</s1><s2>08193 Bellaterra</s2><s3>ESP</s3><sZ>11 aut.</sZ></fA14><fA14 i1="12"><s1>Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904</s1><s2>1098 XH Amsterdam</s2><s3>NLD</s3><sZ>13 aut.</sZ></fA14><fA14 i1="13"><s1>Department of Physics and Astronomy, University of British Colombia, 6224 Agricultural Road</s1><s2>Vancouver, BC V6T 1Z1</s2><s3>CAN</s3><sZ>14 aut.</sZ></fA14><fA14 i1="14"><s1>LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>15 aut.</sZ></fA14><fA14 i1="15"><s1>INAF - Osservatorio Astrofisico di Catania, Via S.Sofia 78</s1><s2>95123 Catania</s2><s3>ITA</s3><sZ>17 aut.</sZ></fA14><fA14 i1="16"><s1>Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>19 aut.</sZ></fA14><fA14 i1="17"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Konkoly Thege Miklos út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>20 aut.</sZ></fA14><fA14 i1="18"><s1>SETI Institute/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>21 aut.</sZ></fA14><fA14 i1="19"><s1>Orbital Sciences Corporation/NASA Ames Research Center</s1><s2>Moffett Field, CA 94035</s2><s3>USA</s3><sZ>22 aut.</sZ><sZ>23 aut.</sZ></fA14><fA20><s1>2077-2088</s1></fA20><fA21><s1>2012</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000506062930180</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>12-0049842</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>USA</s0></fA66><fC01 i1="01" l="ENG"><s0>Mass-loss of red giant branch (RGB) stars is still poorly determined, despite its crucial role in the chemical enrichment of galaxies. Thanks to the recent detection of solar-like oscillations in G-K giants in open clusters with Kepler, we can now directly determine stellar masses for a statistically significant sample of stars in the old open clusters NGC 6791 and 6819. The aim of this work is to constrain the integrated RGB mass-loss by comparing the average mass of stars in the red clump (RC) with that of stars in the low-luminosity portion of the RGB [i.e. stars with L ? L(RC)]. Stellar masses were determined by combining the available seismic parameters v<sub>max</sub> and Δv with additional photometric constraints and with independent distance estimates. We measured the masses of 40 stars on the RGB and 19 in the RC of the old metal-rich cluster NGC 6791. We find that the difference between the average mass of RGB and RC stars is small, but significant [ΔM? = 0.09 ± 0.03 (random) ±0.04 (systematic) M<sub>◦.</sub>]. Interestingly, such a small ΔM? does not support scenarios of an extreme mass-loss for this metal-rich cluster. If we describe the mass-loss rate with Reimers prescription, a first comparison with isochrones suggests that the observed AM? is compatible with a mass-loss efficiency parameter in the range 0.1 ? η ? 0.3. Less stringent constraints on the RGB mass-loss rate are set by the analysis of the ˜2 Gyr old NGC 6819, largely due to the lower mass-loss expected for this cluster, and to the lack of an independent and accurate distance determination. In the near future, additional constraints from frequencies of individual pulsation modes and spectroscopic effective temperatures will allow further stringent tests of the Δv and v<sub>max</sub> scaling relations, which provide a novel, and potentially very accurate, means of determining stellar radii and masses.</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>Amas ouvert</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Open clusters</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>Perte masse</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Mass loss</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Etoile géante</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Giant stars</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Enrichissement chimique</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Chemical enrichment</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Enriquecimiento químico</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Galaxies</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Galaxies</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Masse stellaire</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Stellar mass</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Luminosité</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Luminosity</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Taux perte</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Loss rate</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Porcentaje pérdida</s0><s5>35</s5></fC03><fC03 i1="11" i2="X" l="FRE"><s0>Isochrone</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="ENG"><s0>Isochrone</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="SPA"><s0>Isocrono</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Mesure distance</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Distance measurement</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Température effective</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Effective temperature</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><fC03 i1="15" i2="3" l="FRE"><s0>Amas stellaire</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Star clusters</s0><s5>40</s5></fC03><fN21><s1>030</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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