Hostname: page-component-5c6d5d7d68-xq9c7 Total loading time: 0 Render date: 2024-08-29T16:36:05.312Z Has data issue: false hasContentIssue false
  • English
  • Français

X-ray emission characteristics of an O+O binary HD 93205

Published online by Cambridge University Press:  29 August 2024

Bharti Arora Open the ORCID record for Bharti Arora [Opens in a new window]  and
Jeewan C. Pandey
Bharti Arora*
Affiliation:
Aryabhatta Research Institute of Observational Sciences, Nainital-263 002, Uttarakhand, India School of Studies in Physics & Astrophysics, Pt. Ravishankar Shukla University, Raipur–492 010, India
Jeewan C. Pandey*
Affiliation:
Aryabhatta Research Institute of Observational Sciences, Nainital-263 002, Uttarakhand, India
*
email: bhartiarora612@gmail.com, jeewan@aries.res.in
email: bhartiarora612@gmail.com, jeewan@aries.res.in
Get access Rights & Permissions [Opens in a new window]

Abstract

A detailed X-ray study of a massive binary called HD 93205 has been made using long-term XMM-Newton observations. The X-ray spectrum of HD 93205 displays negligible counts above 5 keV. The two thermal plasma emission models with average temperature values as ∼ 0.20 and ∼ 0.60 keV are required to explain the X-ray spectra. The X-ray flux variations in the binary are noticed to be in qualitative agreement with the wind-wind collision model but with a few deviations from the expected 1/D trend (D is the binary separation).

Keywords

Stars:early-typebinaries:colliding-windsX-rays:starsstars:individual: HD 93205
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 323 - 325
Check for updates
Copyright
© The Author(s), 2024. 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

Antokhin, I. I., Rauw, G., Vreux, J.-M., et al. 2003, Magnetic Fields in O, B and A Stars: Origin and Connection to Pulsation, Rotation and Mass Loss, 305, 383 Google Scholar
Arora, B., Pandey, J. C., & De Becker, M. 2019, MNRAS 487, 2624 Google Scholar
Conti, P. S. & Walborn, N. R. 1976, ApJ, 207, 502 Google Scholar
Jenkins, E. B. 2019, ApJ, 872, 55 Google Scholar
Sota, A., Maz Apellániz, J., Morrell, N. I., et al. 2014, ApJS, 211, 10 Google Scholar
Supplementary material: PDF

Arora and Pandey supplementary material

Arora and Pandey supplementary material

Download Arora and Pandey supplementary material(PDF)
PDF 1.9 MB