Hostname: page-component-848d4c4894-4rdrl Total loading time: 0 Render date: 2024-06-24T00:54:59.880Z Has data issue: false hasContentIssue false
  • English
  • Français

The surprising X-ray emission of Oe stars

Published online by Cambridge University Press:  12 July 2011

Yael Nazé ,
Gregor Rauw  and
Asif ud-Doula
Yael Nazé
Affiliation:
FNRS-ULg, Dept AGO, Allée du 6 Août 17, Bât B5C, B4000-Liège, Belgium, email: naze@astro.ulg.ac.be
Gregor Rauw
Affiliation:
FNRS-ULg, Dept AGO, Allée du 6 Août 17, Bât B5C, B4000-Liège, Belgium, email: naze@astro.ulg.ac.be
Asif ud-Doula
Affiliation:
Penn State Worthington Scranton, 120 Ridge View Drive, Dunmore, PA 18512, USA
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.

Oe stars are thought to represent an extension of the Be phenomenon to higher temperatures. Dedicated XMM observations of HD 155806 revealed a surprising X-ray spectrum: soft character, absence of overluminosity, broad X-ray lines. These properties are fully compatible with the wind-shock model, which usually explains the X-rays from “normal”, single O-type stars. In contrast, some other Oe/Be stars display a completely different behaviour at high energies.

Keywords

X-rays: starsstars: early-typestars: individual (HD 155806)stars: emission-lineBe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 624 - 625
Copyright
Copyright © International Astronomical Union 2011

References

Conti, P. S. & Leep, E. M. 1974, ApJ, 193, 113Google Scholar
Garmany, C. D., Conti, P. S., & Massey, P. 1980, ApJ, 242, 1063CrossRefGoogle Scholar
Hubrig, S., Schöller, M., Schnerr, R. S., González, J. F. et al. 2008, A&A, 490, 793Google Scholar
Nazé, Y., Rauw, G., & Ud-Doula, A. 2010, A&A, 510, A59Google Scholar
Nazé, Y., & Rauw, G. 2010, arXiv, 1002.0546Google Scholar
Negueruela, I., Steele, I. A., & Bernabeu, G. 2004, AN, 325, 749Google Scholar
Petit, V., Fullerton, A. W., Bagnulo, S., Wade, G. A. et al. 2009, in: Strassmeier, K. G., Kosovichev, A. G. & Beckman, J. E. (eds.), Cosmic Magnetic Fields: From Planets, to Stars and Galaxies, IAU Symposium 259, p. 385Google Scholar
Rakowski, C. E., Schulz, N. S., Wolk, S. J., & Testa, P. 2006, ApJ (Letters), 649, L111CrossRefGoogle Scholar
Rauw, G., Nazé, Y., Marique, P. X., De Becker, M. et al. 2007, IBVS 5773Google Scholar
Vink, J. S., Davies, B., Harries, T. J., Oudmaijer, R. D. et al. 2009, A&A, 505, 743Google Scholar