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X-ray spectroscopy of massive stellar winds: previous and ongoing observations of the hot star ζ Pup

Published online by Cambridge University Press:  30 December 2019

N. Miller ,
W. Waldron ,
J. Nichols ,
D. Huenemoerder ,
M. Dahmer ,
R. Ignace ,
J. Lauer ,
A. Moffat ,
Y. Nazé  and
L. Oskinova
...Show all authors
N. Miller
Affiliation:
Department of Physics & Astronomy, University of Wisconsin-Eau Claire, 105 Garfield Avenue, Eau Claire, WI 54701USA
W. Waldron
Affiliation:
Eureka Scientific, Inc., USA
J. Nichols
Affiliation:
Harvard-Smithsonian Center for Astrophysics, USA
D. Huenemoerder
Affiliation:
Massachusetts Institute of Technology, USA
M. Dahmer
Affiliation:
Northrop Grumman, USA
R. Ignace
Affiliation:
East Tennessee State University, USA
J. Lauer
Affiliation:
Harvard-Smithsonian Center for Astrophysics, USA
A. Moffat
Affiliation:
University of Montreal, Canada
Y. Nazé
Affiliation:
Fund for Scientific Research-FNRS, Belgium and University of Liège, Belgium
L. Oskinova
Affiliation:
University of Potsdam, Germany
N. Richardson
Affiliation:
University of Toledo, USA
T. Ramiaramanantsoa
Affiliation:
Arizona State University, USA
T. Shenar
Affiliation:
KU Leuven, Belgium
K. Gayley
Affiliation:
University of Iowa, USA
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Abstract

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The stellar winds of hot stars have an important impact on both stellar and galactic evolution, yet their structure and internal processes are not fully understood in detail. One of the best nearby laboratories for studying such massive stellar winds is the O4I(n)fp star ζ Pup. After briefly discussing existing X-ray observations from Chandra and XMM, we present a simulation of X-ray emission line profile measurements for the upcoming 840 kilosecond Chandra HETGS observation. This simulation indicates that the increased S/N of this new observation will allow several major steps forward in the understanding of massive stellar winds. By measuring X-ray emission line strengths and profiles, we should be able to differentiate between various stellar wind models and map the entire wind structure in temperature and density. This legacy X-ray spectrum of ζ Pup will be a useful benchmark for future X-ray missions.

Keywords

stars: early-typestars: mass lossstars: windsoutflowsX-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 88 - 92
Copyright
© International Astronomical Union 2019 

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