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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
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Abstract

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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

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