Accurate fundamental parameters for 23 bright solar-type stars
Identifieur interne : 008104 ( Main/Merge ); précédent : 008103; suivant : 008105Accurate fundamental parameters for 23 bright solar-type stars
Auteurs : H. Bruntt [France, Australie] ; T. R. Bedding [Australie] ; P.-O. Quirion [Canada, Danemark] ; G. Lo Curto [Chili] ; F. Carrier [Belgique] ; B. Smalley [Royaume-Uni] ; T. H. Dall [Allemagne] ; T. Arentoft [Danemark] ; M. Bazot [Portugal] ; R. P. Butler [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Spectrométrie.
English descriptors
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Abstract
We combine results from interferometry, asteroseismology and spectroscopy to determine accurate fundamental parameters of 23 bright solar-type stars, from spectral type F5 to K2 and luninosity classes III-V. For some stars we can use direct techniques to determine the mass, radius, luminosity and effective temperature, and we compare with indirect methods that rely on photometric calibrations or spectroscopic analyses. We use the asteroseismic information available in the literature to infer an indirect mass with an accuracy of 4-15 per cent. From indirect methods we determine luminosity and radius to 3 per cent. We find evidence that the luminosity from the indirect method is slightly overestimated (≃5 per cent) for the coolest stars, indicating that their bolometric corrections (BCs) are too negative. For Teff we find a slight offset of -40±20 K between the spectroscopic method and the direct method, meaning the spectroscopic temperatures are too high. From the spectroscopic analysis we determine the detailed chemical composition for 13 elements, including Li, C and O. The metallicity ranges from [Fe/H] = -1.7 to +0.4, and there is clear evidence for α-element enhancement in the metal-poor stars. We find no significant offset between the spectroscopic surface gravity and the value from combining asteroseismology with radius estimates. From the spectroscopy we also determine v sin i and we present a new calibration of macroturbulence and microturbulence. From the comparison between the results from the direct and spectroscopic methods we claim that we can determine Teff, log g and [Fe/H] with absolute accuracies of 80 K, 0.08 and 0.07 dex. Photometric calibrations of Strömgren indices provide accurate results for Teff and [Fe/H] but will be more uncertain for distant stars when interstellar reddening becomes important. The indirect methods are important to obtain reliable estimates of the fundamental parameters of relatively faint stars when interferometry cannot be used. This paper is the first to compare direct and indirect methods for a large sample of stars, and we conclude that indirect methods are valid, although slight corrections may be needed.
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Bruntt</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>LESIA, Observatoire de Paris-Meudon</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>1 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>92195 Meudon</wicri:noRegion><wicri:noRegion>Observatoire de Paris-Meudon</wicri:noRegion><wicri:noRegion>92195 Meudon</wicri:noRegion></affiliation><affiliation wicri:level="4"><inist:fA14 i1="02"><s1>Sydney Institute for Astronomy, School of Physics, The University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>Australie</country><placeName><settlement type="city">Sydney</settlement><region type="état">Nouvelle-Galles du Sud</region></placeName><orgName type="university">Université de Sydney</orgName></affiliation></author><author><name sortKey="Bedding, T R" sort="Bedding, T R" uniqKey="Bedding T" first="T. R." last="Bedding">T. R. 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Lo Curto</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>European Southern Observatory, Alonso de Cordova 3107, Vitacura</s1><s2>Santiago</s2><s3>CHL</s3><sZ>4 aut.</sZ></inist:fA14><country>Chili</country><wicri:noRegion>Santiago</wicri:noRegion></affiliation></author><author><name sortKey="Carrier, F" sort="Carrier, F" uniqKey="Carrier F" first="F." last="Carrier">F. Carrier</name><affiliation wicri:level="4"><inist:fA14 i1="06"><s1>Instituut voor Sterrenkunde, Katholieke Universiteit Leuven</s1><s3>BEL</s3><sZ>5 aut.</sZ></inist:fA14><country>Belgique</country><placeName><settlement type="city">Louvain</settlement><region>Région flamande</region><region type="district" nuts="2">Province du Brabant flamand</region></placeName><orgName type="university">Katholieke Universiteit Leuven</orgName></affiliation></author><author><name sortKey="Smalley, B" sort="Smalley, B" uniqKey="Smalley B" first="B." last="Smalley">B. Smalley</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Astrophysics Group, Keele University, Keele</s1><s2>Staffordshire ST5 5BG</s2><s3>GBR</s3><sZ>6 aut.</sZ></inist:fA14><country>Royaume-Uni</country><wicri:noRegion>Staffordshire ST5 5BG</wicri:noRegion></affiliation></author><author><name sortKey="Dall, T H" sort="Dall, T H" uniqKey="Dall T" first="T. H." last="Dall">T. H. Dall</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>European Southern Observatory, Karl SchKarzschild Str. 2</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>7 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching bei München</wicri:noRegion><wicri:noRegion>Karl SchKarzschild Str. 2</wicri:noRegion><wicri:noRegion>85748 Garching bei München</wicri:noRegion></affiliation></author><author><name sortKey="Arentoft, T" sort="Arentoft, T" uniqKey="Arentoft T" first="T." last="Arentoft">T. Arentoft</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, University of Aarhus</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Danemark</country><wicri:noRegion>8000 Aarhus C</wicri:noRegion></affiliation></author><author><name sortKey="Bazot, M" sort="Bazot, M" uniqKey="Bazot M" first="M." last="Bazot">M. Bazot</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Universidade do Porto, Centro de Astrofísica, Rua das Estrelas</s1><s2>4150-762 Porto</s2><s3>PRT</s3><sZ>9 aut.</sZ></inist:fA14><country>Portugal</country><wicri:noRegion>4150-762 Porto</wicri:noRegion></affiliation></author><author><name sortKey="Butler, R P" sort="Butler, R P" uniqKey="Butler R" first="R. P." last="Butler">R. P. Butler</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road NW</s1><s2>Washington, DC 20015-1305</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Washington, DC 20015-1305</wicri:noRegion></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">10-0328272</idno><date when="2010">2010</date><idno type="stanalyst">PASCAL 10-0328272 INIST</idno><idno type="RBID">Pascal:10-0328272</idno><idno type="wicri:Area/PascalFrancis/Corpus">002560</idno><idno type="wicri:Area/PascalFrancis/Curation">003A26</idno><idno type="wicri:Area/PascalFrancis/Checkpoint">002636</idno><idno type="wicri:explorRef" wicri:stream="PascalFrancis" wicri:step="Checkpoint">002636</idno><idno type="wicri:doubleKey">0035-8711:2010:Bruntt H:accurate:fundamental:parameters</idno><idno type="wicri:Area/Main/Merge">008104</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Accurate fundamental parameters for 23 bright solar-type stars</title><author><name sortKey="Bruntt, H" sort="Bruntt, H" uniqKey="Bruntt H" first="H." last="Bruntt">H. Bruntt</name><affiliation wicri:level="3"><inist:fA14 i1="01"><s1>LESIA, Observatoire de Paris-Meudon</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>1 aut.</sZ></inist:fA14><country>France</country><placeName><region type="region" nuts="2">Île-de-France</region><settlement type="city">Meudon</settlement></placeName></affiliation><affiliation wicri:level="4"><inist:fA14 i1="02"><s1>Sydney Institute for Astronomy, School of Physics, The University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>Australie</country><placeName><settlement type="city">Sydney</settlement><region type="état">Nouvelle-Galles du Sud</region></placeName><orgName type="university">Université de Sydney</orgName></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="4"><inist:fA14 i1="02"><s1>Sydney Institute for Astronomy, School of Physics, The University of Sydney</s1><s2>2006 NSW</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14><country>Australie</country><placeName><settlement type="city">Sydney</settlement><region type="état">Nouvelle-Galles du Sud</region></placeName><orgName type="university">Université de Sydney</orgName></affiliation></author><author><name sortKey="Quirion, P O" sort="Quirion, P O" uniqKey="Quirion P" first="P.-O." last="Quirion">P.-O. Quirion</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Canadian Space Agency, 6767 Boulevard de l'Aéroport</s1><s2>Saint-Hubert, Québec J3Y 8Y9</s2><s3>CAN</s3><sZ>3 aut.</sZ></inist:fA14><country>Canada</country><wicri:noRegion>Saint-Hubert, Québec J3Y 8Y9</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, University of Aarhus</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Danemark</country><wicri:noRegion>8000 Aarhus C</wicri:noRegion></affiliation></author><author><name sortKey="Lo Curto, G" sort="Lo Curto, G" uniqKey="Lo Curto G" first="G." last="Lo Curto">G. Lo Curto</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>European Southern Observatory, Alonso de Cordova 3107, Vitacura</s1><s2>Santiago</s2><s3>CHL</s3><sZ>4 aut.</sZ></inist:fA14><country>Chili</country><wicri:noRegion>Santiago</wicri:noRegion></affiliation></author><author><name sortKey="Carrier, F" sort="Carrier, F" uniqKey="Carrier F" first="F." last="Carrier">F. Carrier</name><affiliation wicri:level="4"><inist:fA14 i1="06"><s1>Instituut voor Sterrenkunde, Katholieke Universiteit Leuven</s1><s3>BEL</s3><sZ>5 aut.</sZ></inist:fA14><country>Belgique</country><placeName><settlement type="city">Louvain</settlement><region>Région flamande</region><region type="district" nuts="2">Province du Brabant flamand</region></placeName><orgName type="university">Katholieke Universiteit Leuven</orgName></affiliation></author><author><name sortKey="Smalley, B" sort="Smalley, B" uniqKey="Smalley B" first="B." last="Smalley">B. Smalley</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Astrophysics Group, Keele University, Keele</s1><s2>Staffordshire ST5 5BG</s2><s3>GBR</s3><sZ>6 aut.</sZ></inist:fA14><country>Royaume-Uni</country><wicri:noRegion>Staffordshire ST5 5BG</wicri:noRegion></affiliation></author><author><name sortKey="Dall, T H" sort="Dall, T H" uniqKey="Dall T" first="T. H." last="Dall">T. H. Dall</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>European Southern Observatory, Karl SchKarzschild Str. 2</s1><s2>85748 Garching bei München</s2><s3>DEU</s3><sZ>7 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>85748 Garching bei München</wicri:noRegion><wicri:noRegion>Karl SchKarzschild Str. 2</wicri:noRegion><wicri:noRegion>85748 Garching bei München</wicri:noRegion></affiliation></author><author><name sortKey="Arentoft, T" sort="Arentoft, T" uniqKey="Arentoft T" first="T." last="Arentoft">T. Arentoft</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, University of Aarhus</s1><s2>8000 Aarhus C</s2><s3>DNK</s3><sZ>3 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Danemark</country><wicri:noRegion>8000 Aarhus C</wicri:noRegion></affiliation></author><author><name sortKey="Bazot, M" sort="Bazot, M" uniqKey="Bazot M" first="M." last="Bazot">M. Bazot</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Universidade do Porto, Centro de Astrofísica, Rua das Estrelas</s1><s2>4150-762 Porto</s2><s3>PRT</s3><sZ>9 aut.</sZ></inist:fA14><country>Portugal</country><wicri:noRegion>4150-762 Porto</wicri:noRegion></affiliation></author><author><name sortKey="Butler, R P" sort="Butler, R P" uniqKey="Butler R" first="R. P." last="Butler">R. P. Butler</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road NW</s1><s2>Washington, DC 20015-1305</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Washington, DC 20015-1305</wicri:noRegion></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="2010">2010</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>Bright star</term><term>Chemical composition</term><term>Corrections</term><term>Effective temperature</term><term>Faint star</term><term>Interferometry</term><term>Interstellar reddening</term><term>Luminosity</term><term>Metal-poor stars</term><term>Metallicity</term><term>Solar type star</term><term>Spectral type</term><term>Spectroscopy</term><term>Stellar abundance</term><term>Surface gravity</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Etoile brillante</term><term>Etoile type solaire</term><term>Interférométrie</term><term>Astéroséismologie</term><term>Spectrométrie</term><term>Type spectral</term><term>Luminosité</term><term>Température effective</term><term>Correction</term><term>Composition chimique</term><term>Métallicité</term><term>Etoile pauvre en métal</term><term>Gravité surface</term><term>Rougissement interstellaire</term><term>Etoile faible</term><term>Abondance stellaire</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Spectrométrie</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We combine results from interferometry, asteroseismology and spectroscopy to determine accurate fundamental parameters of 23 bright solar-type stars, from spectral type F5 to K2 and luninosity classes III-V. For some stars we can use direct techniques to determine the mass, radius, luminosity and effective temperature, and we compare with indirect methods that rely on photometric calibrations or spectroscopic analyses. We use the asteroseismic information available in the literature to infer an indirect mass with an accuracy of 4-15 per cent. From indirect methods we determine luminosity and radius to 3 per cent. We find evidence that the luminosity from the indirect method is slightly overestimated (≃5 per cent) for the coolest stars, indicating that their bolometric corrections (BCs) are too negative. For T<sub>eff</sub> we find a slight offset of -40±20 K between the spectroscopic method and the direct method, meaning the spectroscopic temperatures are too high. From the spectroscopic analysis we determine the detailed chemical composition for 13 elements, including Li, C and O. The metallicity ranges from [Fe/H] = -1.7 to +0.4, and there is clear evidence for α-element enhancement in the metal-poor stars. We find no significant offset between the spectroscopic surface gravity and the value from combining asteroseismology with radius estimates. From the spectroscopy we also determine v sin i and we present a new calibration of macroturbulence and microturbulence. From the comparison between the results from the direct and spectroscopic methods we claim that we can determine T<sub>eff</sub>, log g and [Fe/H] with absolute accuracies of 80 K, 0.08 and 0.07 dex. Photometric calibrations of Strömgren indices provide accurate results for T<sub>eff</sub> and [Fe/H] but will be more uncertain for distant stars when interstellar reddening becomes important. The indirect methods are important to obtain reliable estimates of the fundamental parameters of relatively faint stars when interferometry cannot be used. This paper is the first to compare direct and indirect methods for a large sample of stars, and we conclude that indirect methods are valid, although slight corrections may be needed.</div></front></TEI><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>Belgique</li><li>Canada</li><li>Chili</li><li>Danemark</li><li>France</li><li>Portugal</li><li>Royaume-Uni</li><li>États-Unis</li></country><region><li>Nouvelle-Galles du Sud</li><li>Province du Brabant flamand</li><li>Région flamande</li><li>Île-de-France</li></region><settlement><li>Louvain</li><li>Meudon</li><li>Sydney</li></settlement><orgName><li>Katholieke Universiteit Leuven</li><li>Université de Sydney</li></orgName></list><tree><country name="France"><region name="Île-de-France"><name sortKey="Bruntt, H" sort="Bruntt, H" uniqKey="Bruntt H" first="H." last="Bruntt">H. Bruntt</name></region></country><country name="Australie"><region name="Nouvelle-Galles du Sud"><name sortKey="Bruntt, H" sort="Bruntt, H" uniqKey="Bruntt H" first="H." last="Bruntt">H. Bruntt</name></region><name sortKey="Bedding, T R" sort="Bedding, T R" uniqKey="Bedding T" first="T. R." last="Bedding">T. R. Bedding</name></country><country name="Canada"><noRegion><name sortKey="Quirion, P O" sort="Quirion, P O" uniqKey="Quirion P" first="P.-O." last="Quirion">P.-O. Quirion</name></noRegion></country><country name="Danemark"><noRegion><name sortKey="Quirion, P O" sort="Quirion, P O" uniqKey="Quirion P" first="P.-O." last="Quirion">P.-O. Quirion</name></noRegion><name sortKey="Arentoft, T" sort="Arentoft, T" uniqKey="Arentoft T" first="T." last="Arentoft">T. Arentoft</name></country><country name="Chili"><noRegion><name sortKey="Lo Curto, G" sort="Lo Curto, G" uniqKey="Lo Curto G" first="G." last="Lo Curto">G. 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