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A comprehensive empirical investigation of Galactic fast-rotating O-type stars

Published online by Cambridge University Press:  29 August 2024

N. Britavskiy Open the ORCID record for N. Britavskiy [Opens in a new window] ,
G. Holgado Open the ORCID record for G. Holgado [Opens in a new window] ,
S. Simón-Díaz ,
J. Maíz Apellániz Open the ORCID record for J. Maíz Apellániz [Opens in a new window] ,
M. Pantaleoni González ,
Y. Nazé Open the ORCID record for Y. Nazé [Opens in a new window] ,
S. Burssens  and
J. J. Eldridge
N. Britavskiy*
Affiliation:
Université de Liège, Allée du 6 Aout 19c, B-4000 Sart Tilman, Liège, Belgium
G. Holgado
Affiliation:
Centro de Astrobiología, campus ESAC. Villanueva de la Cañada, E-28692, Spain
S. Simón-Díaz
Affiliation:
Instituto de Astrofísica de Canarias. E-38200 La Laguna, Tenerife, Spain
J. Maíz Apellániz
Affiliation:
Centro de Astrobiología, campus ESAC. Villanueva de la Cañada, E-28692, Spain
M. Pantaleoni González
Affiliation:
Centro de Astrobiología, campus ESAC. Villanueva de la Cañada, E-28692, Spain
Y. Nazé
Affiliation:
Université de Liège, Allée du 6 Aout 19c, B-4000 Sart Tilman, Liège, Belgium
S. Burssens
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
J. J. Eldridge
Affiliation:
Department of Physics, University of Auckland, Private Bag 92019, Auckland, New Zealand
*
email: mbritavskiy@uliege.be
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Abstract

Rotation is one of the important parameters affecting the evolution and final fate of massive stars but the origin of fast rotators remains unclear (imprint of the star formation process, result of binary interactions). In this work, we aim at investigating the binary status, photometric variability, and runaway status of a statistically meaningful sample of Galactic fast-rotating O stars. We perform a comprehensive multi-epoch analysis of new high-quality spectroscopic observations gathered by the IACOB and OWN surveys. Notably, we find that the total percentage of spectroscopic binaries in the investigated sample range between 25 and 40%, in agreement with previous finding for the case of O-type stars with lower projected rotational velocities. On the contrary, the fraction of runaway stars among fast rotators (∼35–50%) is significantly higher than in the case of slow rotators (∼20–30%). By combining all these observational results we will evaluate each scenario about the origin of fast rotators.

Keywords

Stars: early typeStars: rotationStars: binaries.
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 236 - 237
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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References

Holgado, G, Simón-Díaz, S., Herrero, A., & Barbá, R. 2022, A&A, accepted.Google Scholar
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de Mink, S. E., Sana, H., Langer, N., Izzard, R. G., & Schneider, F. R. N. 2014, ApJ, 782, 7 Google Scholar