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dc.contributor.author
Martins, F.
dc.contributor.author
Simón Díaz, S.
dc.contributor.author
Barba, Rodolfo Hector
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dc.contributor.author
Gamen, Roberto Claudio
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dc.contributor.author
Elkstrom, S.
dc.date.available
2019-08-28T15:54:22Z
dc.date.issued
2017-03
dc.identifier.citation
Martins, F.; Simón Díaz, S.; Barba, Rodolfo Hector; Gamen, Roberto Claudio; Elkstrom, S.; A study of the effect of rotational mixing on massive stars evolution: Surface abundances of Galactic O7-8 giant stars; EDP Sciences; Astronomy and Astrophysics; 599; 3-2017; 30-44
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/82371
dc.description.abstract
Context. Massive star evolution remains only partly constrained. In particular, the exact role of rotation has been questioned by puzzling properties of OB stars in the Magellanic Clouds. Aims. Our goal is to study the relation between surface chemical composition and rotational velocity, and to test predictions of evolutionary models including rotation. Methods. We have performed a spectroscopic analysis of a sample of fifteen Galactic O7-8 giant stars. This sample is homogeneous in terms of mass, metallicity and evolutionary state. It is made of stars with a wide range of projected rotational velocities. Results. We show that the sample stars are located on the second half of the main sequence, in a relatively narrow mass range (25-40 M · ). Almost all stars with projected rotational velocities above 100 km s -1 have N/C ratios about ten times the initial value. Below 100 km s -1 a wide range of N/C values is observed. The relation between N/C and surface gravity is well reproduced by various sets of models. Some evolutionary models including rotation are also able to consistently explain slowly rotating, highly enriched stars. This is due to differential rotation which efficiently transports nucleosynthesis products and allows the surface to rotate slower than the core. In addition, angular momentum removal by winds amplifies surface braking on the main sequence. Comparison of the surface composition of O7-8 giant stars with a sample of B stars with initial masses about four times smaller reveal that chemical enrichment scales with initial mass, as expected from theory. Conclusions. Although evolutionary models that include rotation face difficulties in explaining the chemical properties of O- and B-type stars at low metallicity, some of them can consistently account for the properties of main-sequence Galactic O stars in the mass range 25-40 M · .
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Stars: Abundances
dc.subject
Stars: Atmospheres
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Stars: Early-Type
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Stars: Fundamental Parameters
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Stars: Massive
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
A study of the effect of rotational mixing on massive stars evolution: Surface abundances of Galactic O7-8 giant stars
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2019-05-23T20:34:52Z
dc.journal.volume
599
dc.journal.pagination
30-44
dc.journal.pais
Francia
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dc.journal.ciudad
Paris
dc.description.fil
Fil: Martins, F.. Université de Montpellier; Francia
dc.description.fil
Fil: Simón Díaz, S.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; España
dc.description.fil
Fil: Barba, Rodolfo Hector. Universidad de La Serena; Chile
dc.description.fil
Fil: Gamen, Roberto Claudio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
dc.description.fil
Fil: Elkstrom, S.. University of Geneva; Suiza
dc.journal.title
Astronomy and Astrophysics
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2017/03/aa29548-16/aa29548-16.html
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/201629548
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