Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-10T09:49:44.741Z Has data issue: false hasContentIssue false
  • English
  • Français

Dependence of Wolf-Rayet wind clumping on the surface temperature

Published online by Cambridge University Press:  29 August 2024

André-Nicolas Chené Open the ORCID record for André-Nicolas Chené [Opens in a new window] ,
Nicole St-Louis Open the ORCID record for Nicole St-Louis [Opens in a new window] ,
Guillaume Lenoir-Craig Open the ORCID record for Guillaume Lenoir-Craig [Opens in a new window] ,
Anthony F. J. Moffat  and
Kenneth Gayley
André-Nicolas Chené*
Affiliation:
Gemini Observatory/NSF’s NOIRLab, 670 N. A‘ohoku Place, Hilo, Hawai‘i, 96720, USA
Nicole St-Louis
Affiliation:
Centre de Recherche en Astrophysique du Québec, Département de physique, Université de Montréal, Complexe des Sciences, Montréal, QC H2V 0B3, Canada
Guillaume Lenoir-Craig
Affiliation:
Centre de Recherche en Astrophysique du Québec, Département de physique, Université de Montréal, Complexe des Sciences, Montréal, QC H2V 0B3, Canada
Anthony F. J. Moffat
Affiliation:
Centre de Recherche en Astrophysique du Québec, Département de physique, Université de Montréal, Complexe des Sciences, Montréal, QC H2V 0B3, Canada
Kenneth Gayley
Affiliation:
Department of Physics and Astronomy, University of Iowa, Iowa City, IA 52242, USA
*
email: andrenicolas.chene@gmail.com
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present our measurements of the amplitude of photometric and spectroscopic variability due to clumping in the wind of Wolf-Rayet (WR) stars. Photometric variability was assessed using TESS light-curves, while spectroscopic variations were obtained from almost 20 years of monitoring of nearly 100 classical (presumably single) stars. Our results show an apparent dependence of the variability amplitude with the stars’ surface temperature and/or terminal velocity. Our interpretation is that it supports the idea that the dominating driver of the clumps in WR winds is a sub-surface convection region.

Keywords

stars: Wolf-Rayetstars: mass losstechniques: photometrictechniques: spectroscopic
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 493 - 495
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Cantiello, M., et al. 2009, A&A, 499, 279 Google Scholar
Chené, A.-N., St-Louis, N., Moffat, A. F. J., & Gayley, K. G. 2020, ApJ, 903, 113 Google Scholar
Hamann, W. R., et al. 2019, A&A, 625, A57 Google Scholar
Lenoir-Craig, G., et al. 2022, ApJ, 925, 79 Google Scholar
Moens, N., Poniatowski, L. G., Hennicker, L., Sundqvist, J. O., El Mellah, I., & Kee, N. D. 2022, arXiv e-prints, arXiv:2203.01108Google Scholar
Robert, C., & Moffat, A. F. J. 1989, ApJ, 343, 902 Google Scholar
Sander, A. A. C., Hamann, W. R., Todt, H., Hainich, R., Shenar, T., Ramachandran, V., & Oskinova, L. M. 2019, A&A, 621, A92 Google Scholar