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The multiplicity of Galactic Wolf-Rayet stars

Published online by Cambridge University Press:  29 August 2024

Karan Dsilva Open the ORCID record for Karan Dsilva [Opens in a new window] ,
Tomer Shenar ,
Hugues Sana Open the ORCID record for Hugues Sana [Opens in a new window]  and
Pablo Marchant
Karan Dsilva*
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
Tomer Shenar
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium Anton Pannekoek Institute for Astronomy, University of Amsterdam, Postbus 94249, 1090 GE Amsterdam, The Netherlands
Hugues Sana
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
Pablo Marchant
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
*
email: karandsilva413@gmail.com
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Abstract

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We present the results of a magnitude-limited spectroscopic survey of Galactic Wolf-Rayet stars with the HERMES spectrograph mounted on the Mercator telescope. Using cross-correlation to measure radial velocities, we measured the observed binary fractions of the Galactic carbon- (WC) and nitrogen-rich (WN) Wolf-Rayet stars to be and . We used Monte-Carlo simulations with a Bayesian framework to derive the intrinsic multiplicity properties and found and . We find that the majority of WN binaries reside in short-period systems, similar to O stars. However, the orbital period distribution of the Galactic WC population peaks at 5000 d, a discrepancy that challenges our current understanding of binary evolution in Wolf-Rayet stars.

Keywords

stars: Wolf-Rayetstars: binariesstars: evolution
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 496 - 498
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

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