The nature of the hard state of Cygnus X-3 |
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| Authors: | L Hjalmarsdotter A A Zdziarski S Larsson V Beckmann M McCollough D C Hannikainen O Vilhu |
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| Institution: | Observatory, PO Box 14, FIN-00014 University of Helsinki, Finland;Stockholm Observatory, Department of Astronomy, AlbaNova University Centre, 10691 Stockholm, Sweden;Copernicus Astronomical Centre, Bartycka 18, 00-716 Warszawa, Poland;INTEGRAL Science Data Centre, Ch. d'Écogia 16, 1290 Versoix, Switzerland;Department of Physics, Joint Centre for Astrophysics, University of Maryland, Baltimore County, MD 21250, USA;Smithsonian Astrophysical Observatory, 60 Garden Street, MS 67, Cambridge, MA 02138-1516, USA |
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| Abstract: | The X-ray binary Cygnus X-3 (Cyg X-3) is a highly variable X-ray source that displays a wide range of observed spectral states. One of the main states is significantly harder than the others, peaking at ∼20 keV, with only a weak low-energy component. Due to the enigmatic nature of this object, hidden inside the strong stellar wind of its Wolf–Rayet companion, it has remained unclear whether this state represents an intrinsic hard state, with truncation of the inner disc, or whether it is just a result of increased local absorption. We study the X-ray light curves from RXTE /ASM and CGRO /BATSE in terms of distributions and correlations of flux and hardness and find several signs of a bimodal behaviour of the accretion flow that are not likely to be the result of increased absorption in a surrounding medium. Using INTEGRAL observations, we model the broad-band spectrum of Cyg X-3 in its apparent hard state. We find that it can be well described by a model of a hard state with a truncated disc, despite the low cut-off energy, provided the accreted power is supplied to the electrons in the inner flow in the form of acceleration rather than thermal heating, resulting in a hybrid electron distribution and a spectrum with a significant contribution from non-thermal Comptonization, usually observed only in soft states. The high luminosity of this non-thermal hard state implies that either the transition takes place at significantly higher L / L E than in the usual advection models, or the mass of the compact object is ≳20 M⊙ , possibly making it the most-massive black hole observed in an X-ray binary in our Galaxy so far. We find that an absorption model as well as a model of almost pure Compton reflection also fit the data well, but both have difficulties explaining other results, in particular the radio/X-ray correlation. |
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| Keywords: | radiation mechanisms: non-thermal gamma-rays: observations X-rays: binaries X-rays: general X-rays: individual: Cygnus X-3 X-rays: stars |
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