Infrared spectroscopic variability of Cygnus X-3 in outburst and quiescence

Fender, R. P.; Hanson, M. M.; Pooley, G. G.

doi:10.1046/j.1365-8711.1999.02726.x

Cited by 54 publications

(29 citation statements)

References 34 publications

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“…This shows that the spectrum of SS 433 resembles the one of a Wolf-Rayet X-ray binary very well and suggests a common physical mechanism at work in both systems. Indeed a disc-like wind, though significantly flattened in the plane of the binary orbit, has been invoked by Fender et al (1999) to explain both the variability of the He i emission lines in this object and an asymmetric emitting region. This binary system has a much smaller size (∼5 R separation, 4.8 h period) than SS 433 (13 d period), thus the IR emitting region is significantly larger than the binary separation, consequently the outflowing wind is external to the binary orbit.…”

Section: Mass Loss Evaluationmentioning

confidence: 90%

SS 433: a phenomenon imitating a Wolf-Rayet star

Fuchs

Miramond

Ábrahám

2006

A&A

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We present mid-infrared (2-12 µm) spectra of the microquasar SS 433 obtained with the Infrared Space Observatory (spectroscopic mode of ISOPHOT and ISOCAM). We compare them to the spectra of four Wolf-Rayet stars: WR 78, WR 134, WR 136, and WR 147 in the same wavelength range. The mid-infrared spectrum of SS 433 mainly shows H i and He i emission lines and is very similar to the spectrum of WR 147, a WN8(h)+B0.5V binary. The 2-12 µm continuum emission of SS 433 corresponds to optically thin and partially optically thick free-free emission, from which we calculate a mass loss rate of 2−3 × 10 −4 M yr −1 if the wind is homogeneous and a third of these values if it is clumped. This is consistent with a strong stellar wind from a WN star. However, following recent studies concluding that the mass donor star of SS 433 is not a Wolf-Rayet star, we propose that this strong wind out flows from a geometrically thick envelope of material that surrounds the compact object like a stellar atmosphere, imitating the Wolf-Rayet phenomenon. This wind could also wrap the mass donor star, and at larger distances (∼40 AU), it might form a dust envelope from which the thermal emission, detected with ISOPHOT at 25 µm and 60 µm, would originate. This wind also probably feeds the material that is ejected in the orbital plane of the binary system and that forms the equatorial outflow detected in radio at distances > 100 AU.

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Section: Mass Loss Evaluationmentioning

confidence: 90%

SS 433: a phenomenon imitating a Wolf-Rayet star

Fuchs

Miramond

Ábrahám

2006

A&A

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“…Nakamura et al (1993) explain the X-ray spectra as obtained by the Ginga observatory by proposing the presence of three species of ionized gas, fully ionized, almost fully ionized and nearly ionized, engulfing the binary system. Fender et al (1999) suggest a WR type wind with the geometry of a disc in the binary plane with a size much bigger than the binary system to be the origin of the binary modulated He emission lines (obtained from infra-red spectra). This wind originates from the companion which is a WN type Wolf-Rayet star.…”

Section: The Binary Template and Its Stabilitymentioning

confidence: 93%

“…• of Fender et al 1999). The phase resolved spectra of the various Fe emission lines (6.4 keV, 6.7 keV and 6.9 keV) and the absorption edges (7.1 keV and 9.1 keV) during both low-hard and high-soft states may provide better constraints on the origin of the Fe emission lines.…”

Section: The Binary Template and Its Stabilitymentioning

confidence: 99%

Binary corrected X-ray light curve of Cygnus X-3: Implications for the timing properties of the compact binary system

Choudhury

Rao

Vadawale

et al. 2004

A&A

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Abstract. We study the binary corrected X-ray light curve of Cygnus X-3 using the RXTE-ASM (All Sky Monitor) data and RXTE-PCA data. We find that the X-ray template derived from the EXOSAT observations adequately explains the binary variations. Using the recently determined quadratic binary ephemeris we correct the RXTE-PCA lightcurve and obtain the power spectrum which shows distinct features of shifting towards the low frequency regime vis-a-vis the Galactic X-ray binaries. The power spectrum doesn't vary from the hard to the soft state. We also obtain the binary corrected RXTE-ASM monitoring lightcurve and examine the previously obtained correlation between soft X-ray (2−12 keV from RXTE ASM), hard X-ray (20−100 keV from CGRO−BATSE) and radio (2.2 GHz from GBI) after the binary correction. We find that the correlation time scale is less than a day.

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“…The compact star is either a neutron star or a black hole and the companion is a WN5-7 type Wolf-Rayet (WR) star (van Kerkwijk 1992(van Kerkwijk , 1996, with strong evidence pointing to an early-type WN star (Fender et al 1999). The system appears to be engulfed in an extended envelope produced by the wind of the WR star.…”

Section: Introductionmentioning

confidence: 99%

Orbital modulation of X-ray emission lines in Cygnus X-3

Vilhu

Hakala

Hannikainen

et al. 2009

A&A

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Aims. We address the problem where the X-ray emission lines are formed and investigate orbital dynamics using Chandra HETG observations, photoionizing calculations and numerical wind-particle simulations. The aims were to set constraints on the masses of the components of this close binary system consisting of a Wolf-Rayet (WR) star and a compact component and to investigate the nature of the latter (neutron star or black hole). The goal was also to investigate P Cygni signatures in line profiles.Methods. The observed Si xiv (6.185 Å) and S xvi (4.733 Å) line profiles at four orbital phases were fitted with P Cygni-type profiles consisting of an emission and a blue-shifted absorption component. Numerical models were constructed using photoionizing calculations and particle simulations. In the models, the emission originates in the photoionized wind of the WR companion illuminated by a hybrid source: the X-ray radiation of the compact star and the photospheric EUV-radiation from the WR star.Results. Spectral lines with moderate excitation (such as Si xiv and S xvi) arise in the photoionized wind. The emission component exhibits maximum blue-shift at phase 0.5 (when the compact star is in front), while the velocity of the absorption component is constant (around −900 km s −1 ). Both components, like the continuum flux, have intensity maxima around phase 0.5. The simulated Fe xxvi Lyα line (1.78 Å, H-like) from the wind is weak compared to the observed one. We suggest that it originates in the vicinity of the compact star, with a maximum blue shift at phase 0.25 (compact star approaching). By combining the mass function derived with that from the infrared He i absorption (arising from the WR companion), we constrain the masses and the inclination of the system. Conclusions. The Si xiv and S xvi lines and their radial velocity curves can be understood in the framework of a photoionized wind involving a hybrid ionizer. Constraints on the compact star mass and orbital inclination (i) are given using the mass functions derived from the Fe xxvi line and He i 2.06 μm absorption. Both a neutron star at large inclination (i ≥ 60 degrees) and a black hole at small inclination are possible solutions. The radial velocity amplitude of the He ii 2.09 μm emission (formed in the X-ray shadow behind the WR star) suggests i = 30 degrees, implying a possible compact star mass between 2.8-8.0 M . For i = 60 degrees the same range is 1.0-3.2 M .

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Infrared spectroscopic variability of Cygnus X-3 in outburst and quiescence

Cited by 54 publications

References 34 publications

SS 433: a phenomenon imitating a Wolf-Rayet star

SS 433: a phenomenon imitating a Wolf-Rayet star

Binary corrected X-ray light curve of Cygnus X-3: Implications for the timing properties of the compact binary system

Orbital modulation of X-ray emission lines in Cygnus X-3

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