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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: matheus.bernini@uni-heidelberg.de
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Abstract

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
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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