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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: [email protected], [email protected]
email: [email protected], [email protected]
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Abstract

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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
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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
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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
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