Accurate fundamental parameters for 23 bright solar-type stars
Identifieur interne : 002560 ( PascalFrancis/Corpus ); précédent : 002559; suivant : 002561Accurate fundamental parameters for 23 bright solar-type stars
Auteurs : H. Bruntt ; T. R. Bedding ; P.-O. Quirion ; G. Lo Curto ; F. Carrier ; B. Smalley ; T. H. Dall ; T. Arentoft ; M. Bazot ; R. P. ButlerSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010.
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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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| NO : | PASCAL 10-0328272 INIST |
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| ET : | Accurate fundamental parameters for 23 bright solar-type stars |
| AU : | BRUNTT (H.); BEDDING (T. R.); QUIRION (P.-O.); LO CURTO (G.); CARRIER (F.); SMALLEY (B.); DALL (T. H.); ARENTOFT (T.); BAZOT (M.); BUTLER (R. P.) |
| AF : | LESIA, Observatoire de Paris-Meudon/92195 Meudon/France (1 aut.); Sydney Institute for Astronomy, School of Physics, The University of Sydney/2006 NSW/Australie (1 aut., 2 aut.); Canadian Space Agency, 6767 Boulevard de l'Aéroport/Saint-Hubert, Québec J3Y 8Y9/Canada (3 aut.); Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, University of Aarhus/8000 Aarhus C/Danemark (3 aut., 8 aut.); European Southern Observatory, Alonso de Cordova 3107, Vitacura/Santiago/Chili (4 aut.); Instituut voor Sterrenkunde, Katholieke Universiteit Leuven/Belgique (5 aut.); Astrophysics Group, Keele University, Keele/Staffordshire ST5 5BG/Royaume-Uni (6 aut.); European Southern Observatory, Karl SchKarzschild Str. 2/85748 Garching bei München/Allemagne (7 aut.); Universidade do Porto, Centro de Astrofísica, Rua das Estrelas/4150-762 Porto/Portugal (9 aut.); Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road NW/Washington, DC 20015-1305/Etats-Unis (10 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2010; Vol. 405; No. 3; Pp. 1907-1923; Bibl. 1 p.1/4 |
| LA : | Anglais |
| EA : | 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. |
| CC : | 001E03 |
| FD : | Etoile brillante; Etoile type solaire; Interférométrie; Astéroséismologie; Spectrométrie; Type spectral; Luminosité; Température effective; Correction; Composition chimique; Métallicité; Etoile pauvre en métal; Gravité surface; Rougissement interstellaire; Etoile faible; Abondance stellaire |
| ED : | Bright star; Solar type star; Interferometry; Astroseismology; Spectroscopy; Spectral type; Luminosity; Effective temperature; Corrections; Chemical composition; Metallicity; Metal-poor stars; Surface gravity; Interstellar reddening; Faint star; Stellar abundance |
| SD : | Estrella brillante; Estrella tipo solar; Tipo espectral; Metalicidad; Estrella débil; Abundancia estelar |
| LO : | INIST-2067.354000193165130360 |
| ID : | 10-0328272 |
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Butler</name><affiliation><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></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></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><inist:fA14 i1="01"><s1>LESIA, Observatoire de Paris-Meudon</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>1 aut.</sZ></inist:fA14></affiliation><affiliation><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></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="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></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><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></affiliation><affiliation><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></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><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></affiliation></author><author><name sortKey="Carrier, F" sort="Carrier, F" uniqKey="Carrier F" first="F." last="Carrier">F. Carrier</name><affiliation><inist:fA14 i1="06"><s1>Instituut voor Sterrenkunde, Katholieke Universiteit Leuven</s1><s3>BEL</s3><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Smalley, B" sort="Smalley, B" uniqKey="Smalley B" first="B." last="Smalley">B. Smalley</name><affiliation><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></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><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></affiliation></author><author><name sortKey="Arentoft, T" sort="Arentoft, T" uniqKey="Arentoft T" first="T." last="Arentoft">T. Arentoft</name><affiliation><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></affiliation></author><author><name sortKey="Bazot, M" sort="Bazot, M" uniqKey="Bazot M" first="M." last="Bazot">M. Bazot</name><affiliation><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></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><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></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></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><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>405</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Accurate fundamental parameters for 23 bright solar-type stars</s1></fA08><fA11 i1="01" i2="1"><s1>BRUNTT (H.)</s1></fA11><fA11 i1="02" i2="1"><s1>BEDDING (T. R.)</s1></fA11><fA11 i1="03" i2="1"><s1>QUIRION (P.-O.)</s1></fA11><fA11 i1="04" i2="1"><s1>LO CURTO (G.)</s1></fA11><fA11 i1="05" i2="1"><s1>CARRIER (F.)</s1></fA11><fA11 i1="06" i2="1"><s1>SMALLEY (B.)</s1></fA11><fA11 i1="07" i2="1"><s1>DALL (T. H.)</s1></fA11><fA11 i1="08" i2="1"><s1>ARENTOFT (T.)</s1></fA11><fA11 i1="09" i2="1"><s1>BAZOT (M.)</s1></fA11><fA11 i1="10" i2="1"><s1>BUTLER (R. P.)</s1></fA11><fA14 i1="01"><s1>LESIA, Observatoire de Paris-Meudon</s1><s2>92195 Meudon</s2><s3>FRA</s3><sZ>1 aut.</sZ></fA14><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></fA14><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></fA14><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></fA14><fA14 i1="05"><s1>European Southern Observatory, Alonso de Cordova 3107, Vitacura</s1><s2>Santiago</s2><s3>CHL</s3><sZ>4 aut.</sZ></fA14><fA14 i1="06"><s1>Instituut voor Sterrenkunde, Katholieke Universiteit Leuven</s1><s3>BEL</s3><sZ>5 aut.</sZ></fA14><fA14 i1="07"><s1>Astrophysics Group, Keele University, Keele</s1><s2>Staffordshire ST5 5BG</s2><s3>GBR</s3><sZ>6 aut.</sZ></fA14><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></fA14><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></fA14><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></fA14><fA20><s1>1907-1923</s1></fA20><fA21><s1>2010</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000193165130360</s5></fA43><fA44><s0>0000</s0><s1>© 2010 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1 p.1/4</s0></fA45><fA47 i1="01" i2="1"><s0>10-0328272</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>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.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Etoile brillante</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Bright star</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Estrella brillante</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Etoile type solaire</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Solar type star</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Estrella tipo solar</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Interférométrie</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Interferometry</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Astéroséismologie</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Astroseismology</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Spectrométrie</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Spectroscopy</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Type spectral</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Spectral type</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Tipo espectral</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Luminosité</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Luminosity</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Température effective</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Effective temperature</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Correction</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Corrections</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Composition chimique</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Chemical composition</s0><s5>35</s5></fC03><fC03 i1="11" i2="X" l="FRE"><s0>Métallicité</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="ENG"><s0>Metallicity</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="SPA"><s0>Metalicidad</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Etoile pauvre en métal</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Metal-poor stars</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Gravité surface</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Surface gravity</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Rougissement interstellaire</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Interstellar reddening</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Etoile faible</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Faint star</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Estrella débil</s0><s5>40</s5></fC03><fC03 i1="16" i2="X" l="FRE"><s0>Abondance stellaire</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="ENG"><s0>Stellar abundance</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="SPA"><s0>Abundancia estelar</s0><s5>41</s5></fC03><fN21><s1>207</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 10-0328272 INIST</NO><ET>Accurate fundamental parameters for 23 bright solar-type stars</ET><AU>BRUNTT (H.); BEDDING (T. R.); QUIRION (P.-O.); LO CURTO (G.); CARRIER (F.); SMALLEY (B.); DALL (T. H.); ARENTOFT (T.); BAZOT (M.); BUTLER (R. P.)</AU><AF>LESIA, Observatoire de Paris-Meudon/92195 Meudon/France (1 aut.); Sydney Institute for Astronomy, School of Physics, The University of Sydney/2006 NSW/Australie (1 aut., 2 aut.); Canadian Space Agency, 6767 Boulevard de l'Aéroport/Saint-Hubert, Québec J3Y 8Y9/Canada (3 aut.); Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, University of Aarhus/8000 Aarhus C/Danemark (3 aut., 8 aut.); European Southern Observatory, Alonso de Cordova 3107, Vitacura/Santiago/Chili (4 aut.); Instituut voor Sterrenkunde, Katholieke Universiteit Leuven/Belgique (5 aut.); Astrophysics Group, Keele University, Keele/Staffordshire ST5 5BG/Royaume-Uni (6 aut.); European Southern Observatory, Karl SchKarzschild Str. 2/85748 Garching bei München/Allemagne (7 aut.); Universidade do Porto, Centro de Astrofísica, Rua das Estrelas/4150-762 Porto/Portugal (9 aut.); Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road NW/Washington, DC 20015-1305/Etats-Unis (10 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2010; Vol. 405; No. 3; Pp. 1907-1923; Bibl. 1 p.1/4</SO><LA>Anglais</LA><EA>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.</EA><CC>001E03</CC><FD>Etoile brillante; Etoile type solaire; Interférométrie; Astéroséismologie; Spectrométrie; Type spectral; Luminosité; Température effective; Correction; Composition chimique; Métallicité; Etoile pauvre en métal; Gravité surface; Rougissement interstellaire; Etoile faible; Abondance stellaire</FD><ED>Bright star; Solar type star; Interferometry; Astroseismology; Spectroscopy; Spectral type; Luminosity; Effective temperature; Corrections; Chemical composition; Metallicity; Metal-poor stars; Surface gravity; Interstellar reddening; Faint star; Stellar abundance</ED><SD>Estrella brillante; Estrella tipo solar; Tipo espectral; Metalicidad; Estrella débil; Abundancia estelar</SD><LO>INIST-2067.354000193165130360</LO><ID>10-0328272</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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