AustralieFrV1, Main, Exploration, bibRecord, 005965

RESOLVING VEGA AND THE INCLINATION CONTROVERSY WITH CHARA/MIRC

Identifieur interne : 005965 ( Main/Exploration ); précédent : 005964; suivant : 005966

RESOLVING VEGA AND THE INCLINATION CONTROVERSY WITH CHARA/MIRC

Auteurs : J. D. Monnier [États-Unis] ; XIAO CHE [États-Unis] ; MING ZHAO [États-Unis] ; S. Ekström [Suisse] ; V. Maestro [Australie] ; Jason Aufdenberg [États-Unis] ; F. Baron [États-Unis] ; C. Georgy [France] ; S. Kraus [États-Unis] ; H. Mcalister [États-Unis] ; E. Pedretti [Royaume-Uni] ; S. Ridgway [États-Unis] ; J. Sturmann [États-Unis] ; L. Sturmann [États-Unis] ; T. Ten Brummelaar [États-Unis] ; N. Thureau [Royaume-Uni] ; N. Turner [États-Unis] ; P. G. Tuthill [Australie]

Source :

The Astrophysical journal [ 0004-637X ] ; 2012.

RBID : Pascal:13-0029872

Descripteurs français

Pascal (Inist)
- Rotation rapide, Etoile rotation, Profil raie, Gravité, Modèle, Champ magnétique, Age, Métallicité, Incertitude, Etoile IR, Rotation stellaire.

English descriptors

KwdEn :
- Age, Gravity, Infrared star, Line shape, Magnetic fields, Metallicity, Models, Rapid rotation, Rotating star, Stellar rotation, Uncertainty.

Abstract

Optical and infrared interferometers definitively established that the photometric standard Vega (= α Lyrae) is a rapidly rotating star viewed nearly pole-on. Recent independent spectroscopic analyses could not reconcile the inferred inclination angle with the observed line profiles, preferring a larger inclination. In order to resolve this controversy, we observed Vega using the six-beam Michigan Infrared Combiner on the Center for High Angular Resolution Astronomy Array. With our greater angular resolution and dense (u, v)-coverage, we find that Vega is rotating less rapidly and with a smaller gravity darkening coefficient than previous interferometric results. Our models are compatible with low photospheric macroturbulence and are also consistent with the possible rotational period of ∼0.71 days recently reported based on magnetic field observations. Our updated evolutionary analysis explicitly incorporates rapid rotation, finding Vega to have a mass of 2.15^+0.10_-0.15 M_◦. and an age 700^-75₊₁₅₀ Myr, substantially older than previous estimates with errors dominated by lingering metallicity uncertainties (_Z = 0.006^+0.003_-0.002).

Affiliations:

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Le document en format XML

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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">RESOLVING VEGA AND THE INCLINATION CONTROVERSY WITH CHARA/MIRC</title>
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<sZ>10 aut.</sZ>
<sZ>13 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
<wicri:noRegion>The CHARA Array of Georgia State University</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Sturmann, L" sort="Sturmann, L" uniqKey="Sturmann L" first="L." last="Sturmann">L. Sturmann</name>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>The CHARA Array of Georgia State University</s1>
<s2>Mt. Wilson, CA, 91023</s2>
<s3>USA</s3>
<sZ>10 aut.</sZ>
<sZ>13 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
<wicri:noRegion>The CHARA Array of Georgia State University</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Ten Brummelaar, T" sort="Ten Brummelaar, T" uniqKey="Ten Brummelaar T" first="T." last="Ten Brummelaar">T. Ten Brummelaar</name>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>The CHARA Array of Georgia State University</s1>
<s2>Mt. Wilson, CA, 91023</s2>
<s3>USA</s3>
<sZ>10 aut.</sZ>
<sZ>13 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
<wicri:noRegion>The CHARA Array of Georgia State University</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Thureau, N" sort="Thureau, N" uniqKey="Thureau N" first="N." last="Thureau">N. Thureau</name>
<affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Department of Physics and Astronomy, University of St. Andrews</s1>
<s3>GBR</s3>
<sZ>16 aut.</sZ>
</inist:fA14>
<country>Royaume-Uni</country>
<wicri:noRegion>Department of Physics and Astronomy, University of St. Andrews</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Turner, N" sort="Turner, N" uniqKey="Turner N" first="N." last="Turner">N. Turner</name>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>The CHARA Array of Georgia State University</s1>
<s2>Mt. Wilson, CA, 91023</s2>
<s3>USA</s3>
<sZ>10 aut.</sZ>
<sZ>13 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
<wicri:noRegion>The CHARA Array of Georgia State University</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Tuthill, P G" sort="Tuthill, P G" uniqKey="Tuthill P" first="P. G." last="Tuthill">P. G. Tuthill</name>
<affiliation wicri:level="4"><inist:fA14 i1="04"><s1>Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney</s1>
<s2>NSW 2006</s2>
<s3>AUS</s3>
<sZ>5 aut.</sZ>
<sZ>18 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>
</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="2012">2012</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>Age</term>
<term>Gravity</term>
<term>Infrared star</term>
<term>Line shape</term>
<term>Magnetic fields</term>
<term>Metallicity</term>
<term>Models</term>
<term>Rapid rotation</term>
<term>Rotating star</term>
<term>Stellar rotation</term>
<term>Uncertainty</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Rotation rapide</term>
<term>Etoile rotation</term>
<term>Profil raie</term>
<term>Gravité</term>
<term>Modèle</term>
<term>Champ magnétique</term>
<term>Age</term>
<term>Métallicité</term>
<term>Incertitude</term>
<term>Etoile IR</term>
<term>Rotation stellaire</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">Optical and infrared interferometers definitively established that the photometric standard Vega (= α Lyrae) is a rapidly rotating star viewed nearly pole-on. Recent independent spectroscopic analyses could not reconcile the inferred inclination angle with the observed line profiles, preferring a larger inclination. In order to resolve this controversy, we observed Vega using the six-beam Michigan Infrared Combiner on the Center for High Angular Resolution Astronomy Array. With our greater angular resolution and dense (u, v)-coverage, we find that Vega is rotating less rapidly and with a smaller gravity darkening coefficient than previous interferometric results. Our models are compatible with low photospheric macroturbulence and are also consistent with the possible rotational period of ∼0.71 days recently reported based on magnetic field observations. Our updated evolutionary analysis explicitly incorporates rapid rotation, finding Vega to have a mass of 2.15<sup>+0.10</sup>
<sub>-0.15</sub>
 M<sub>◦.</sub>
 and an age 700<sup>-75</sup>
<sub>+150</sub>
 Myr, substantially older than previous estimates with errors dominated by lingering metallicity uncertainties (<sub>Z</sub>
 = 0.006<sup>+0.003</sup>
<sub>-0.002</sub>
).</div>
</front>
</TEI>
<affiliations><list><country><li>Australie</li>
<li>France</li>
<li>Royaume-Uni</li>
<li>Suisse</li>
<li>États-Unis</li>
</country>
<region><li>Auvergne-Rhône-Alpes</li>
<li>Canton de Genève</li>
<li>Nouvelle-Galles du Sud</li>
<li>Pennsylvanie</li>
<li>Rhône-Alpes</li>
</region>
<settlement><li>Genève</li>
<li>Lyon</li>
<li>Sydney</li>
<li>University Park (Pennsylvanie)</li>
</settlement>
<orgName><li>Université d'État de Pennsylvanie</li>
<li>Université de Genève</li>
<li>Université de Sydney</li>
</orgName>
</list>
<tree><country name="États-Unis"><noRegion><name sortKey="Monnier, J D" sort="Monnier, J D" uniqKey="Monnier J" first="J. D." last="Monnier">J. D. Monnier</name>
</noRegion>
<name sortKey="Aufdenberg, Jason" sort="Aufdenberg, Jason" uniqKey="Aufdenberg J" first="Jason" last="Aufdenberg">Jason Aufdenberg</name>
<name sortKey="Baron, F" sort="Baron, F" uniqKey="Baron F" first="F." last="Baron">F. Baron</name>
<name sortKey="Kraus, S" sort="Kraus, S" uniqKey="Kraus S" first="S." last="Kraus">S. Kraus</name>
<name sortKey="Mcalister, H" sort="Mcalister, H" uniqKey="Mcalister H" first="H." last="Mcalister">H. Mcalister</name>
<name sortKey="Ming Zhao" sort="Ming Zhao" uniqKey="Ming Zhao" last="Ming Zhao">MING ZHAO</name>
<name sortKey="Ridgway, S" sort="Ridgway, S" uniqKey="Ridgway S" first="S." last="Ridgway">S. Ridgway</name>
<name sortKey="Sturmann, J" sort="Sturmann, J" uniqKey="Sturmann J" first="J." last="Sturmann">J. Sturmann</name>
<name sortKey="Sturmann, L" sort="Sturmann, L" uniqKey="Sturmann L" first="L." last="Sturmann">L. Sturmann</name>
<name sortKey="Ten Brummelaar, T" sort="Ten Brummelaar, T" uniqKey="Ten Brummelaar T" first="T." last="Ten Brummelaar">T. Ten Brummelaar</name>
<name sortKey="Turner, N" sort="Turner, N" uniqKey="Turner N" first="N." last="Turner">N. Turner</name>
<name sortKey="Xiao Che" sort="Xiao Che" uniqKey="Xiao Che" last="Xiao Che">XIAO CHE</name>
</country>
<country name="Suisse"><region name="Canton de Genève"><name sortKey="Ekstrom, S" sort="Ekstrom, S" uniqKey="Ekstrom S" first="S." last="Ekström">S. Ekström</name>
</region>
</country>
<country name="Australie"><region name="Nouvelle-Galles du Sud"><name sortKey="Maestro, V" sort="Maestro, V" uniqKey="Maestro V" first="V." last="Maestro">V. Maestro</name>
</region>
<name sortKey="Tuthill, P G" sort="Tuthill, P G" uniqKey="Tuthill P" first="P. G." last="Tuthill">P. G. Tuthill</name>
</country>
<country name="France"><region name="Auvergne-Rhône-Alpes"><name sortKey="Georgy, C" sort="Georgy, C" uniqKey="Georgy C" first="C." last="Georgy">C. Georgy</name>
</region>
</country>
<country name="Royaume-Uni"><noRegion><name sortKey="Pedretti, E" sort="Pedretti, E" uniqKey="Pedretti E" first="E." last="Pedretti">E. Pedretti</name>
</noRegion>
<name sortKey="Thureau, N" sort="Thureau, N" uniqKey="Thureau N" first="N." last="Thureau">N. Thureau</name>
</country>
</tree>
</affiliations>
</record>

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RESOLVING VEGA AND THE INCLINATION CONTROVERSY WITH CHARA/MIRC

RESOLVING VEGA AND THE INCLINATION CONTROVERSY WITH CHARA/MIRC

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