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The X-ray spectral and timing properties of a major radio flare episode in Cygnus X-3

Published online by Cambridge University Press:  21 February 2013

Karri I. I. Koljonen ,
Diana C. Hannikainen ,
Michael L. McCollough ,
Guy G. Pooley ,
Sergei A. Trushkin  and
Robert Droulans
Karri I. I. Koljonen
Affiliation:
Aalto University Metsähovi Radio Observatory, Metsähovintie 114, 02540 Kylmälä, Finland email: karri@kurp.hut.fi
Diana C. Hannikainen
Affiliation:
Department of Physics and Space Sciences, Florida Institute of Technology, 150 W. University Blvd., Melbourne, FL 32901, USA
Michael L. McCollough
Affiliation:
Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USA
Guy G. Pooley
Affiliation:
Astrophysics Group, Cavendish Laboratory, 19 J. J. Thomson Avenue, Cambridge, UK
Sergei A. Trushkin
Affiliation:
Special Astrophysical Observarory RAS, Nizhnij Arkhyz, 36916, Russia
Robert Droulans
Affiliation:
CNRS; IRAP; 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
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Abstract

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The microquasar Cygnus X-3 is known for massive outbursts that emit radiation from radio to γ-rays associated with jet ejection events. Using Principal Component Analysis to probe fast (~1 min) X-ray spectral evolution followed by subsequent spectral fits to the time-averaged spectra (~3 ks), we find that the overall X-ray variability during major outbursts can be attributed to two components. The spectral evolution of these components are best fitted with hybrid Comptonization and thermal bremsstrahlung components. Most of the X-ray variability is attributed to the hybrid Comptonization component. However, the spectral evolution of the thermal component is linked to a change in the X-ray spectral state. Phase-folding the fit results shows that the thermal component is restricted to two orbital phase regions opposite to each other, possibly indicating a flattened stellar wind from the Wolf-Rayet companion.

Keywords

Accretionaccretion disks – Binaries: close – Stars: windsoutflows – X-rays: binaries – X-rays: individual: Cygnus X-3
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 237 - 238
Copyright
Copyright © International Astronomical Union 2013

References

Belmont, R., Malzac, J., & Marcowith, A. 2008, A&A, 491, 617Google Scholar
Koljonen, K. I. I.et al. 2010, MNRAS, 406, 307CrossRefGoogle Scholar
Malzac, J.et al. 2006, A&A, 448, 1125Google Scholar
Mineo, T.et al. 2012, A&A, 537, 18Google Scholar
Seifina, E. & Titarchuk, L. 2010, ApJ, 722, 586CrossRefGoogle Scholar
Titarchuk, L. & Seifina, E. 2009, ApJ, 706, 1463CrossRefGoogle Scholar
Zdziarski, A. A., Misra, R., & Gierlinski, M. 2010, MNRAS, 402, 767CrossRefGoogle Scholar
Zṿcki, P. T., Done, C., & Smith, D. A. 2001, MNRAS, 326, 1367Google Scholar