Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-22T21:16:57.387Z Has data issue: false hasContentIssue false
  • English
  • Français

Clumping and X-rays in cool B-Supergiants

Published online by Cambridge University Press:  29 August 2024

Matheus Bernini-Peron ,
W. L. F. Marcolino  and
A. A. C. Sander
Matheus Bernini-Peron*
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut Mönchhofstr. 12-14, 69120, Heidelberg, Germany
W. L. F. Marcolino
Affiliation:
Observatório do Valongo, Federal University of Rio de Janeiro, Ladeira do Pedro Antônio, 20080-090, Rio de Janeiro, Brazil
A. A. C. Sander
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut Mönchhofstr. 12-14, 69120, Heidelberg, Germany
*
email: [email protected]
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.

B supergiants (BSGs) lie on the cool end of line-driven wind regime, such that the study of their atmospheres can help us to understand the physics of line-driven winds. So far key features of their spectra, especially in the UV region, could not be reproduced consistently with atmosphere models. This represents a significant gap in our knowledge of their physical properties and behavior, which is particularly striking for BSGs on the cool side of the Bi-Stability Jump (cooler than B1). To address this problem, we analysed a sample of Galactic cool BSGs, with sufficient UV and optical coverage. None of our targets are detected in X-rays with only upper limits existing for some of them.

Keywords

massive starsstellar windsB-supergiantclumpingX-rayBi-stability
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 182 - 183
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481Google Scholar
Berghoefer, T. W., Schmitt, J. H. M. M., Danner, R., & Cassinelli, J. P. 1997, A&A, 322, 167Google Scholar
Cantiello, M., Langer, N., Brott, I., et al. 2009, A&A, 499, 279Google Scholar
Crowther, P. A., Lennon, D. J., & Walborn, N. R. 2006, A&A, 446, 279Google Scholar
Driessen, F. A., Sundqvist, J. O., & Kee, N. D. 2019, A&A, 631, A172Google Scholar
Lamers, H. J. G. L. M., Snow, T. P., & Lindholm, D. M. 1995, ApJ, 455, 269CrossRefGoogle Scholar
Nazé, Y. 2009, A&A, 506, 1055Google Scholar
Oskinova, L. M., Hamann, W. R., & Feldmeier, A. 2007, A&A, 476, 1331Google Scholar
Petrov, B., Vink, J. S., & Gräfener, G. 2014, A&A, 565, A62Google Scholar
Prinja, R. K. & Massa, D. L. 2010, A&A, 521, L55Google Scholar
Rubio-Díez, M. M., Sundqvist, J. O., Najarro, F., et al. 2022, A&A, 658, A61Google Scholar
Searle, S. C., Prinja, R. K., Massa, D., & Ryans, R. 2008, A&A, 481, 777Google Scholar
Vink, J. S., de Koter, A., & Lamers, H. J. G. L. M. 2000, A&A, 362, 295 Google Scholar