Hostname: page-component-848d4c4894-xm8r8 Total loading time: 0 Render date: 2024-06-17T17:20:22.439Z Has data issue: false hasContentIssue false
  • English
  • Français

X-ray view of colliding winds in WR 25

Published online by Cambridge University Press:  16 August 2023

Bharti Arora Open the ORCID record for Bharti Arora [Opens in a new window] ,
Jeewan C. Pandey  and
Michaël De Becker
Bharti Arora
Affiliation:
Aryabhatta Research Institute of Observational Sciences, Nainital-263 002, Uttarakhand, India
Jeewan C. Pandey
Affiliation:
Aryabhatta Research Institute of Observational Sciences, Nainital-263 002, Uttarakhand, India
Michaël De Becker
Affiliation:
Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Liège, Quartier Agora, 19c, Allée du 6 Aôut, B5c, B-4000 Sart Tilman, Belgium
Get access Rights & Permissions [Opens in a new window]

Astract

The long-term behavior of a colliding wind binary WR 25 is presented using archival X-ray data obtained over a time span of : 16 years. The present analysis reveals phase-locked variations repeating consistently over many consecutive orbits of the source (with binary orbital period : 208 days). A significant deviation of the X-ray flux with respect to the theoretical 1/D trend (D is the binary separation) close to periastron passage has been observed. This may occur due to the shifting of the adiabatic wind collision to the radiative regime in that part of the orbit. Further, no signature of X-ray emission in 10.0-79.0 keV energy range attributable to inverse Compton scattering is detected by NuSTAR.

Keywords

Stars:early-typebinaries:colliding-windsX-rays:starsstars:individual: WR 25
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S370: Winds of Stars and Exoplanets , August 2021 , pp. 230 - 231
Check for updates
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Arora, B., Pandey, J. C., & De Becker, M. 2019, MNRAS, 487, 2624 10.1093/mnras/stz1447CrossRefGoogle Scholar
Crowther, P. A. & Walborn, N. R. 2011, MNRAS, 416, 1311 10.1111/j.1365-2966.2011.19129.xCrossRefGoogle Scholar
De Becker, M. & Raucq, F. 2013, A&A, 558, A28 10.1051/0004-6361/201322074CrossRefGoogle Scholar
Gamen, R., Gosset, E., Morrell, N., et al. 2006, A&A, 460, 777 10.1051/0004-6361:20065618CrossRefGoogle Scholar
Pandey, J. C., Pandey, S. B., & Karmakar, S. 2014, ApJ, 788, 84 10.1088/0004-637X/788/1/84CrossRefGoogle Scholar