PittsburghV1, PascalFrancis, Corpus, bibRecord, 003581

Properties of Galactic early-type O-supergiants A combined FUV-UV and optical analysis

Identifieur interne : 003581 ( PascalFrancis/Corpus ); précédent : 003580; suivant : 003582

Properties of Galactic early-type O-supergiants A combined FUV-UV and optical analysis

Auteurs : J.-C. Bouret ; D. J. Hillier ; T. Lanz ; A. W. Fullerton

Source :

Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.

RBID : Pascal:12-0411601

Descripteurs français

Pascal (Inist)
- Supergéante, Type spectral, Perte masse, Taux perte, Etoile O, Distribution vent, Ecart équilibre thermodynamique local, Température effective, Luminosité, Gravité surface, Abondance, Facteur remplissage, Age, Etoile massive, Isochrone, Masse stellaire, Composition chimique, Modèle, Mélangeage, Rotateur, Etoile premier type, Vent stellaire, Evolution stellaire.

English descriptors

KwdEn :
- Abundance, Age, Chemical composition, Early type stars, Effective temperature, Fill factor, Isochrone, Loss rate, Luminosity, Mass loss, Massive stars, Mixing, Models, Non-LTE, O stars, Rotator, Spectral type, Stellar evolution, Stellar mass, Stellar winds, Supergiant stars, Surface gravity, Wind field.

Abstract

Aims. We aim to constrain the properties and evolutionary status of early and mid-spectral type supergiants (from 04 to O7.5). These posses the highest mass-loss rates among the O stars, and exhibit conspicuous wind profiles. Methods. Using the non-LTE wind code C_MFGEN we simultaneously analyzed the FUV-UV and optical spectral range to determine the photospheric properties and wind parameters. We derived effective temperatures, luminosities, surface gravities, surface abundances, mass-loss rates, wind terminal velocities, and clumping filling factors. Results. The supergiants define a very clear evolutionary sequence, in terms of ages and masses, from younger and more massive stars to older stars with lower initial masses. O4 supergiants cluster around the 3 Myr isochrone and are more massive than 60 M_◦., while the O5 to 07.5 stars have masses in the range 50-40 M_o and are 4 ± 0.3 Myr old. The surface chemical composition is typical of evolved O supergiants (nitrogen-rich, carbon- and oxygen-poor). While the observed ranges of carbon and nitrogen mass-fractions are compatible with those expected from evolutionary models for the measured stellar masses, the N/C ratios as a function of age are inconsistent with the theoretical predictions for the four earliest (O4 spectral type) stars of the sample. We question the efficiency of rotational mixing as a function of age for these stars and suggest that another mechanism may be needed to explain the observed abundance patterns. Mass-loss rates derived with clumped-models range within a factor of three of the theoretical mass-loss rates. The corresponding volume-filling factors associated with small-scale clumping are 0.05 ± 0.02. Clumping is found to start close to the photosphere for all but three stars, two of which are fast rotators.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A14	`02`			`@1 Department of Physics and Astronomy, University of Pittsburgh @2 Pittsburgh, PA 15260 @3 USA @Z 2 aut.`
A14	`03`			`@1 Laboratoire J.-L. Lagrange, UMR 7293, Universite de Nice-Sophia Antipolis, CNRS, Observatoire de la Cote d'Azur, BP 4229 @2 06304 Nice @3 FRA @Z 3 aut.`
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Format Inist (serveur)

NO :	PASCAL 12-0411601 INIST
ET :	Properties of Galactic early-type O-supergiants A combined FUV-UV and optical analysis
AU :	BOURET (J.-C.); HILLIER (D. J.); LANZ (T.); FULLERTON (A. W.)
AF :	Laboratoire d'Astrophysique de Marseille, Université d'Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie/13388 Marseille/France (1 aut.); Department of Physics and Astronomy, University of Pittsburgh/Pittsburgh, PA 15260/Etats-Unis (2 aut.); Laboratoire J.-L. Lagrange, UMR 7293, Universite de Nice-Sophia Antipolis, CNRS, Observatoire de la Cote d'Azur, BP 4229/06304 Nice/France (3 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (4 aut.)
DT :	Publication en série; Niveau analytique
SO :	Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2012; Vol. 544; No. p. 1; A67.1-A67.30; Bibl. 1 p.
LA :	Anglais
EA :	Aims. We aim to constrain the properties and evolutionary status of early and mid-spectral type supergiants (from 04 to O7.5). These posses the highest mass-loss rates among the O stars, and exhibit conspicuous wind profiles. Methods. Using the non-LTE wind code C_MFGEN we simultaneously analyzed the FUV-UV and optical spectral range to determine the photospheric properties and wind parameters. We derived effective temperatures, luminosities, surface gravities, surface abundances, mass-loss rates, wind terminal velocities, and clumping filling factors. Results. The supergiants define a very clear evolutionary sequence, in terms of ages and masses, from younger and more massive stars to older stars with lower initial masses. O4 supergiants cluster around the 3 Myr isochrone and are more massive than 60 M_◦., while the O5 to 07.5 stars have masses in the range 50-40 M_o and are 4 ± 0.3 Myr old. The surface chemical composition is typical of evolved O supergiants (nitrogen-rich, carbon- and oxygen-poor). While the observed ranges of carbon and nitrogen mass-fractions are compatible with those expected from evolutionary models for the measured stellar masses, the N/C ratios as a function of age are inconsistent with the theoretical predictions for the four earliest (O4 spectral type) stars of the sample. We question the efficiency of rotational mixing as a function of age for these stars and suggest that another mechanism may be needed to explain the observed abundance patterns. Mass-loss rates derived with clumped-models range within a factor of three of the theoretical mass-loss rates. The corresponding volume-filling factors associated with small-scale clumping are 0.05 ± 0.02. Clumping is found to start close to the photosphere for all but three stars, two of which are fast rotators.
CC :	001E03
FD :	Supergéante; Type spectral; Perte masse; Taux perte; Etoile O; Distribution vent; Ecart équilibre thermodynamique local; Température effective; Luminosité; Gravité surface; Abondance; Facteur remplissage; Age; Etoile massive; Isochrone; Masse stellaire; Composition chimique; Modèle; Mélangeage; Rotateur; Etoile premier type; Vent stellaire; Evolution stellaire
ED :	Supergiant stars; Spectral type; Mass loss; Loss rate; O stars; Wind field; Non-LTE; Effective temperature; Luminosity; Surface gravity; Abundance; Fill factor; Age; Massive stars; Isochrone; Stellar mass; Chemical composition; Models; Mixing; Rotator; Early type stars; Stellar winds; Stellar evolution
SD :	Tipo espectral; Porcentaje pérdida; Distribución viento; Edad; Isocrono; Modelo; Rotador
LO :	INIST-14176.354000506819240610
ID :	12-0411601

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Pascal:12-0411601

Le document en format XML

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<front><div type="abstract" xml:lang="en">Aims. We aim to constrain the properties and evolutionary status of early and mid-spectral type supergiants (from 04 to O7.5). These posses the highest mass-loss rates among the O stars, and exhibit conspicuous wind profiles. Methods. Using the non-LTE wind code C<sub>MFGE</sub>
N we simultaneously analyzed the FUV-UV and optical spectral range to determine the photospheric properties and wind parameters. We derived effective temperatures, luminosities, surface gravities, surface abundances, mass-loss rates, wind terminal velocities, and clumping filling factors. Results. The supergiants define a very clear evolutionary sequence, in terms of ages and masses, from younger and more massive stars to older stars with lower initial masses. O4 supergiants cluster around the 3 Myr isochrone and are more massive than 60 M<sub>◦.</sub>
, while the O5 to 07.5 stars have masses in the range 50-40 M<sub>o</sub>
 and are 4 ± 0.3 Myr old. The surface chemical composition is typical of evolved O supergiants (nitrogen-rich, carbon- and oxygen-poor). While the observed ranges of carbon and nitrogen mass-fractions are compatible with those expected from evolutionary models for the measured stellar masses, the N/C ratios as a function of age are inconsistent with the theoretical predictions for the four earliest (O4 spectral type) stars of the sample. We question the efficiency of rotational mixing as a function of age for these stars and suggest that another mechanism may be needed to explain the observed abundance patterns. Mass-loss rates derived with clumped-models range within a factor of three of the theoretical mass-loss rates. The corresponding volume-filling factors associated with small-scale clumping are 0.05 ± 0.02. Clumping is found to start close to the photosphere for all but three stars, two of which are fast rotators.</div>
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<fA47 i1="01" i2="1"><s0>12-0411601</s0>
</fA47>
<fA60><s1>P</s1>
</fA60>
<fA61><s0>A</s0>
</fA61>
<fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0>
</fA64>
<fA66 i1="01"><s0>FRA</s0>
</fA66>
<fC01 i1="01" l="ENG"><s0>Aims. We aim to constrain the properties and evolutionary status of early and mid-spectral type supergiants (from 04 to O7.5). These posses the highest mass-loss rates among the O stars, and exhibit conspicuous wind profiles. Methods. Using the non-LTE wind code C<sub>MFGE</sub>
N we simultaneously analyzed the FUV-UV and optical spectral range to determine the photospheric properties and wind parameters. We derived effective temperatures, luminosities, surface gravities, surface abundances, mass-loss rates, wind terminal velocities, and clumping filling factors. Results. The supergiants define a very clear evolutionary sequence, in terms of ages and masses, from younger and more massive stars to older stars with lower initial masses. O4 supergiants cluster around the 3 Myr isochrone and are more massive than 60 M<sub>◦.</sub>
, while the O5 to 07.5 stars have masses in the range 50-40 M<sub>o</sub>
 and are 4 ± 0.3 Myr old. The surface chemical composition is typical of evolved O supergiants (nitrogen-rich, carbon- and oxygen-poor). While the observed ranges of carbon and nitrogen mass-fractions are compatible with those expected from evolutionary models for the measured stellar masses, the N/C ratios as a function of age are inconsistent with the theoretical predictions for the four earliest (O4 spectral type) stars of the sample. We question the efficiency of rotational mixing as a function of age for these stars and suggest that another mechanism may be needed to explain the observed abundance patterns. Mass-loss rates derived with clumped-models range within a factor of three of the theoretical mass-loss rates. The corresponding volume-filling factors associated with small-scale clumping are 0.05 ± 0.02. Clumping is found to start close to the photosphere for all but three stars, two of which are fast rotators.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Supergéante</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Supergiant stars</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="X" l="FRE"><s0>Type spectral</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="ENG"><s0>Spectral type</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="SPA"><s0>Tipo espectral</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="3" l="FRE"><s0>Perte masse</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="3" l="ENG"><s0>Mass loss</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="X" l="FRE"><s0>Taux perte</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="ENG"><s0>Loss rate</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="SPA"><s0>Porcentaje pérdida</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE"><s0>Etoile O</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG"><s0>O stars</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="X" l="FRE"><s0>Distribution vent</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="ENG"><s0>Wind field</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="SPA"><s0>Distribución viento</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE"><s0>Ecart équilibre thermodynamique local</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG"><s0>Non-LTE</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>Luminosité</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Luminosity</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE"><s0>Gravité surface</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG"><s0>Surface gravity</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Abondance</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Abundance</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="3" l="FRE"><s0>Facteur remplissage</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="3" l="ENG"><s0>Fill factor</s0>
<s5>37</s5>
</fC03>
<fC03 i1="13" i2="X" l="FRE"><s0>Age</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="ENG"><s0>Age</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="SPA"><s0>Edad</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="3" l="FRE"><s0>Etoile massive</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="3" l="ENG"><s0>Massive stars</s0>
<s5>39</s5>
</fC03>
<fC03 i1="15" i2="X" l="FRE"><s0>Isochrone</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="X" l="ENG"><s0>Isochrone</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="X" l="SPA"><s0>Isocrono</s0>
<s5>40</s5>
</fC03>
<fC03 i1="16" i2="3" l="FRE"><s0>Masse stellaire</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="3" l="ENG"><s0>Stellar mass</s0>
<s5>41</s5>
</fC03>
<fC03 i1="17" i2="3" l="FRE"><s0>Composition chimique</s0>
<s5>42</s5>
</fC03>
<fC03 i1="17" i2="3" l="ENG"><s0>Chemical composition</s0>
<s5>42</s5>
</fC03>
<fC03 i1="18" i2="X" l="FRE"><s0>Modèle</s0>
<s5>43</s5>
</fC03>
<fC03 i1="18" i2="X" l="ENG"><s0>Models</s0>
<s5>43</s5>
</fC03>
<fC03 i1="18" i2="X" l="SPA"><s0>Modelo</s0>
<s5>43</s5>
</fC03>
<fC03 i1="19" i2="3" l="FRE"><s0>Mélangeage</s0>
<s5>44</s5>
</fC03>
<fC03 i1="19" i2="3" l="ENG"><s0>Mixing</s0>
<s5>44</s5>
</fC03>
<fC03 i1="20" i2="X" l="FRE"><s0>Rotateur</s0>
<s5>45</s5>
</fC03>
<fC03 i1="20" i2="X" l="ENG"><s0>Rotator</s0>
<s5>45</s5>
</fC03>
<fC03 i1="20" i2="X" l="SPA"><s0>Rotador</s0>
<s5>45</s5>
</fC03>
<fC03 i1="21" i2="3" l="FRE"><s0>Etoile premier type</s0>
<s5>46</s5>
</fC03>
<fC03 i1="21" i2="3" l="ENG"><s0>Early type stars</s0>
<s5>46</s5>
</fC03>
<fC03 i1="22" i2="3" l="FRE"><s0>Vent stellaire</s0>
<s5>47</s5>
</fC03>
<fC03 i1="22" i2="3" l="ENG"><s0>Stellar winds</s0>
<s5>47</s5>
</fC03>
<fC03 i1="23" i2="3" l="FRE"><s0>Evolution stellaire</s0>
<s5>48</s5>
</fC03>
<fC03 i1="23" i2="3" l="ENG"><s0>Stellar evolution</s0>
<s5>48</s5>
</fC03>
<fN21><s1>317</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
<server><NO>PASCAL 12-0411601 INIST</NO>
<ET>Properties of Galactic early-type O-supergiants A combined FUV-UV and optical analysis</ET>
<AU>BOURET (J.-C.); HILLIER (D. J.); LANZ (T.); FULLERTON (A. W.)</AU>
<AF>Laboratoire d'Astrophysique de Marseille, Université d'Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie/13388 Marseille/France (1 aut.); Department of Physics and Astronomy, University of Pittsburgh/Pittsburgh, PA 15260/Etats-Unis (2 aut.); Laboratoire J.-L. Lagrange, UMR 7293, Universite de Nice-Sophia Antipolis, CNRS, Observatoire de la Cote d'Azur, BP 4229/06304 Nice/France (3 aut.); Space Telescope Science Institute, 3700 San Martin Drive/Baltimore, MD 21218/Etats-Unis (4 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2012; Vol. 544; No. p. 1; A67.1-A67.30; Bibl. 1 p.</SO>
<LA>Anglais</LA>
<EA>Aims. We aim to constrain the properties and evolutionary status of early and mid-spectral type supergiants (from 04 to O7.5). These posses the highest mass-loss rates among the O stars, and exhibit conspicuous wind profiles. Methods. Using the non-LTE wind code C<sub>MFGE</sub>
N we simultaneously analyzed the FUV-UV and optical spectral range to determine the photospheric properties and wind parameters. We derived effective temperatures, luminosities, surface gravities, surface abundances, mass-loss rates, wind terminal velocities, and clumping filling factors. Results. The supergiants define a very clear evolutionary sequence, in terms of ages and masses, from younger and more massive stars to older stars with lower initial masses. O4 supergiants cluster around the 3 Myr isochrone and are more massive than 60 M<sub>◦.</sub>
, while the O5 to 07.5 stars have masses in the range 50-40 M<sub>o</sub>
 and are 4 ± 0.3 Myr old. The surface chemical composition is typical of evolved O supergiants (nitrogen-rich, carbon- and oxygen-poor). While the observed ranges of carbon and nitrogen mass-fractions are compatible with those expected from evolutionary models for the measured stellar masses, the N/C ratios as a function of age are inconsistent with the theoretical predictions for the four earliest (O4 spectral type) stars of the sample. We question the efficiency of rotational mixing as a function of age for these stars and suggest that another mechanism may be needed to explain the observed abundance patterns. Mass-loss rates derived with clumped-models range within a factor of three of the theoretical mass-loss rates. The corresponding volume-filling factors associated with small-scale clumping are 0.05 ± 0.02. Clumping is found to start close to the photosphere for all but three stars, two of which are fast rotators.</EA>
<CC>001E03</CC>
<FD>Supergéante; Type spectral; Perte masse; Taux perte; Etoile O; Distribution vent; Ecart équilibre thermodynamique local; Température effective; Luminosité; Gravité surface; Abondance; Facteur remplissage; Age; Etoile massive; Isochrone; Masse stellaire; Composition chimique; Modèle; Mélangeage; Rotateur; Etoile premier type; Vent stellaire; Evolution stellaire</FD>
<ED>Supergiant stars; Spectral type; Mass loss; Loss rate; O stars; Wind field; Non-LTE; Effective temperature; Luminosity; Surface gravity; Abundance; Fill factor; Age; Massive stars; Isochrone; Stellar mass; Chemical composition; Models; Mixing; Rotator; Early type stars; Stellar winds; Stellar evolution</ED>
<SD>Tipo espectral; Porcentaje pérdida; Distribución viento; Edad; Isocrono; Modelo; Rotador</SD>
<LO>INIST-14176.354000506819240610</LO>
<ID>12-0411601</ID>
</server>
</inist>
</record>

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Properties of Galactic early-type O-supergiants A combined FUV-UV and optical analysis

Properties of Galactic early-type O-supergiants A combined FUV-UV and optical analysis

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