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X-ray diagnostics of massive star winds

Published online by Cambridge University Press:  28 July 2017

L. M. Oskinova ,
R. Ignace  and
D. P. Huenemoerder
L. M. Oskinova
Affiliation:
Institut für Physik und Astronomie, Universität Potsdam, Germany
R. Ignace
Affiliation:
Department of Physics and Astronomy, East Tennessee State University, TN 37663, USA
D. P. Huenemoerder
Affiliation:
Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research, 70 Vassar St., Cambridge, MA 02139, USA
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Abstract

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Observations with powerful X-ray telescopes, such as XMM-Newton and Chandra, significantly advance our understanding of massive stars. Nearly all early-type stars are X-ray sources. Studies of their X-ray emission provide important diagnostics of stellar winds. High-resolution X-ray spectra of O-type stars are well explained when stellar wind clumping is taking into account, providing further support to a modern picture of stellar winds as non-stationary, inhomogeneous outflows. X-ray variability is detected from such winds, on time scales likely associated with stellar rotation. High-resolution X-ray spectroscopy indicates that the winds of late O-type stars are predominantly in a hot phase. Consequently, X-rays provide the best observational window to study these winds. X-ray spectroscopy of evolved, Wolf-Rayet type, stars allows to probe their powerful metal enhanced winds, while the mechanisms responsible for the X-ray emission of these stars are not yet understood.

Keywords

stars: atmospheresstars: early-typestars: mass lossstars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 151 - 155
Copyright
Copyright © International Astronomical Union 2017 

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