New measurements of orbital period change in Cygnus X-3

Singh, Nilkamal; Naik, Sachindra; Paul, Biswajit; Agrawal, P. C.; Rao, A. R.; Singh, Keisham Surjit

doi:10.1051/0004-6361:20020923

Cited by 59 publications

(97 citation statements)

References 20 publications

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“…The 4.8 h X-ray light curve has shown a remarkable stability in terms of its shape (Ghosh et al 1981) and the period has shown a gradual increase at a rate of ∼10 −9 s s −1 . Recently, Singh et al (2002) have extended the span of the observation and have concluded that the period change is consistent with a constant rate of 5.76 ± 0.24 × 10 −10 . Remarkably, the binary modulation was also found to be consistent with the template derived from the EXOSAT data (van der Klis & Bonnet-Bidaud 1989).…”

Section: Introductionmentioning

confidence: 86%

“…Recently, Singh et al (2002) have extended the data base of the binary period measurements using the Indian X-ray Astronomy Experiment (IXAE) and archival data from ROSAT, ASCA, BeppoSAX and RXTE. They found that the binary template obtained from the EXOSAT data adequately explains the recent observations and have derived a value of the period derivative of 5.76 ± 0.24 × 10 −10 .…”

Section: Binary Correctionmentioning

confidence: 99%

“…Inclusion of second derivative marginally improved the fit, essentially giving an upper limit to the second derivative (P = −1.3 ± 1.6 × 10 −11 yr −1 ). We have folded the RXTE ASM data using the quadratic ephemeris of Singh et al (2002) from MJD 50 410 to MJD 51 400 (P = 0.19968443 d;Ṗ = 5.76 × 10 −10 ; time of zero phase T 0 = 2 440 949.892 JD). The time span chosen for the folding corresponds to the data used by Choudhury et al (2003) for the detailed X-ray, radio and hard X-ray correlation analysis.…”

Section: Binary Correctionmentioning

confidence: 99%

“…1. The X-ray light curve of Cygnus X-3 obtained from RXTE-ASM for the period of MJD 50 410 to 51 400 folded at the quadratic ephemeris given by Singh et al (2002). The template data obtained from EXOSAT (van der Klis & Bonnet-Bidaud 1989) is also shown, with appropriate scaling for the count rates.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Introductionmentioning

confidence: 86%

Section: Binary Correctionmentioning

confidence: 99%

Section: Binary Correctionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…The ephemeris of Singh et al (2002) was used to compute the orbits. The data were limited to moderately high states (daily means ≥15 counts/s), to be more consistent with the Cygnus X-3 spectral state during the Chandra/HETG observations used.…”

Section: Modeling Of the X-ray Continuum And Emission Line Light Curvesmentioning

confidence: 99%

Modeling the X-ray light curves of Cygnus X-3

Vilhu

Hannikainen

2013

A&A

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Context. We address the physics behind the soft X-ray light curve asymmetries in Cygnus X-3, a well-known microquasar. Aims. Observable effects of the jet close to the line-of-sight were investigated and interpreted within the frame of light curve physics. Methods. The path of a hypothetical imprint of the jet, advected by the Wolf-Rayet-wind, was computed and its crossing with the lineof-sight during the binary orbit determined. We explored the possibility that physically this "imprint" is a formation of dense clumps triggered by jet bow shocks in the wind ("clumpy trail"). Models for X-ray continuum and emission line light curves were constructed using two absorbers: mass columns along the line-of-sight of i) the WR wind and ii) the clumpy trail, as seen from the compact star. These model light curves were compared with the observed ones from the RXTE/ASM (continuum) and Chandra/HETG (emission lines). Results. We show that the shapes of the Cyg X-3 light curves can be explained by the two absorbers using the inclination and true anomaly angles of the jet as derived from gamma-ray Fermi/LAT observations. The clumpy trail absorber is much larger for the lines than for the continuum. We suggest that the clumpy trail is a mixture of equilibrium and hot (shock heated) clumps. Conclusions. A possible way for studying jets in binary stars when the jet axis and the line-of-sight are close to each other is demonstrated. The X-ray continuum and emission line light curves of Cygnus X-3 can be explained by two absorbers: the WR companion wind plus an absorber lying in the jet path (clumpy trail). We propose that the clumpy trail absorber is due to dense clumps triggered by jet bow shocks.

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Cyg X‐3: A gamma‐ray binary

Sinitsyna

2021

Astron Nachr

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Cygnus X-3 (Cyg X-3) is the famous binary system containing a black hole. It is actively studied through the wide range of electromagnetic spectra from radio band up to ultrahigh energies. Cyg X-3 has long been considered an object for very high energy gamma-ray observations. We present the results of more than 20-year-long studies of Cyg X-3 in the range of 800 GeV to 100 TeV with the SHALON telescope. The detected TeV γ-ray source was identified with Cyg X-3 based on the detection of the γ-ray flux modulation during the orbital period of this binary system of 4.8 hr. The detected modulation of TeV γ-ray emission with orbit, together with the high luminosity of the companion star of Cyg X-3 and the close orbit, leads to the efficient generation of the part of γ-ray emission in the inverse Compton scattering. The correlation of TeV flux increases with the flaring activity of Cyg X-3 in X-ray and radio ranges is found, which could be associated with powerful mass ejections from the central regions around the black hole.

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New measurements of orbital period change in Cygnus X-3

Cited by 59 publications

References 20 publications

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

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

Modeling the X-ray light curves of Cygnus X-3

Cyg X‐3: A gamma‐ray binary

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