Hostname: page-component-cd9895bd7-8ctnn Total loading time: 0 Render date: 2024-12-26T04:16:59.506Z Has data issue: false hasContentIssue false
  • English
  • Français

High-resolution X-ray imaging of the colliding wind shock in WR 147 (WN8(h)+B0.5V)

Published online by Cambridge University Press:  26 May 2016

Julian M. Pittard ,
Ian R. Stevens ,
Peredur M. Williams ,
Andrew M.T. Pollock ,
Steven L. Skinner ,
Michael F. Corcoran  and
Anthony F.J. Moffat
Julian M. Pittard
Affiliation:
Department of Physics and Astronomy, The University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
Ian R. Stevens
Affiliation:
School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
Peredur M. Williams
Affiliation:
Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, Scotland
Andrew M.T. Pollock
Affiliation:
Computer & Sci. Co. Ltd., 230 Graham Rd., Sheffield, S10 3GS, UK
Steven L. Skinner
Affiliation:
Center for Astrophysics and Space Astronomy, University of Colorado, UCB 389, Boulder, CO 80309, USA
Michael F. Corcoran
Affiliation:
Universities Space Research Association, 7501 Forbes Blvd, Ste 206, Seabrook, MD 20706, USA Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
Anthony F.J. Moffat
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succ. Centre-Ville, QC H3C 3J7, Canada

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.

We present the results of a high-resolution Chandra X-ray image of the Wolf-Rayet binary system WR 147, which consists of a WN8 star and an early-type companion located 0″.6 to its north. The image provides the first direct evidence for spatially extended X-ray emission in an early-type binary system, and shows that the emission peaks north of the WN8 star and close to the position of the radio bow shock. Simulated X-ray images of the wind-wind collision have a fwhm consistent with the data, but cannot account for the full spatial extension, unless emission from the stars is also included.

Type
Part 1. Atmospheres of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 222 - 223
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Cherepashchuk, A.M. 1976, Pis'ma Astron. Zh. 2, 356 (= Soviet Astron. Letters 2, 138).Google Scholar
Lépine, S., Wallace, D.J., Shara, M.M., et al. 2001, AJ 122, 3407.Google Scholar
Niemela, V.S., Shara, M.M., Wallace, D.J., et al. 1998, AJ 115, 2047.CrossRefGoogle Scholar
Pittard, J.M., Stevens, I.R., Williams, P.M., et al. 2002, A&A 388, 335.Google Scholar
Prilutskii, O.F., Usov, V.V. 1976, Astron. Zh. 53, 6 (= Soviet Astron. 20, 2).Google Scholar
Williams, P.M., Dougherty, S.M., Davis, R.J., et al. 1997, MNRAS 289, 10.Google Scholar