The 1982 September radio outburst of Cygnus X-3 - Evidence for jetlike emission expanding at not less than about 0.35 C

Geldzahler, B. J.; Johnston, K. J.; Spencer, J. H.; Klepczyński, W. J.; Josties, F. J.; Angerhofer, P. E.; Florkowski, D. R.; McCarthy, Dennis D.; Matsakis, Demetrios; Hjellming, R. M.

doi:10.1086/184131

Cited by 57 publications

(29 citation statements)

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“…Simple arguments show that the twin‐peaked emission lines cannot arise directly from material in the relativistic outflows which are inferred from high‐resolution radio mapping of Cyg X‐3 (e.g. Geldzahler et al 1983; Mioduszewski et al 1998). First, the persistently stronger red wing as shown in Fig.…”

Section: Discussionmentioning

confidence: 99%

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

Fender

Hanson

Pooley³

1999

Monthly Notices of the Royal Astronomical Society

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We present four epochs of high‐resolution infrared spectroscopy of the peculiar X‐ray binary Cygnus X‐3. The observations cover quiescent, small‐flaring and outburst states of the system as defined by radio and X‐ray monitoring. The underlying infrared spectrum of the source, as observed during radio and X‐ray quiescence and small‐flaring states, is one of broad, weak He ii and N v emission. Spectral variability in this state is dominated by modulation at the 4.8‐h orbital period of the system. H‐band spectra confirm the significant hydrogen depletion of the mass donor. The closest spectral match to the quiescent infrared spectrum of Cyg X‐3 is an early‐type WN Wolf–Rayet star. In outburst, the infrared spectrum is dramatically different, with the appearance of very strong twin‐peaked He i emission displaying both day‐to‐day variability and V(iolet)/R(ed) variations with orbital phase. We argue that the twin‐peaked emission cannot arise in relativistic jets or, unless the distance to Cyg X‐3 is severely overestimated, an accretion disc. The most likely explanation appears to be an enhanced stellar wind from the companion. Thus X‐ray and radio outbursts in this system are likely to originate in mass‐transfer, and not disc, instabilities, and the lengthening of the orbital period will not be smooth but will be accelerated during these outbursts. Furthermore, the appearance of these lines is suggestive of an asymmetric emitting region. We propose that the wind in Cyg X‐3 is significantly flattened in the plane of the binary orbit. This may explain the observed twin‐peaked He i features as well as reconciling a massive Wolf–Rayet secondary with the relatively small optical depth to X‐rays, if the disc wind is inclined at some angle to the line of sight. A small set of observations following outburst, when the system was returning to a more quiescent X‐ray and radio state, reveal strong He i 2.058‐μm absorption with a clear P Cygni profile, at the same time as the more common weak He ii and N v features. In a disc‐wind geometry this can be interpreted as absorption in the densest, accelerating regions of the wind which can be viewed directly if the disc is inclined at some angle to the line of sight.

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Section: Discussionmentioning

confidence: 99%

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

Fender

Hanson

Pooley³

1999

Monthly Notices of the Royal Astronomical Society

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“…The previous two decades of interferometric observations suggested symmetric double or triple radio source structures, always with moderate relativistic velocities (∼0.3c). The works by Geldzahler et al (1983), Spencer et al (1986) and Schalinski et al (1995) are good examples of such a statement. It is true that these historical interpretations were sometimes based on model fitting analysis using a limited number of baselines in the array.…”

Section: A One-sided Versus a Two-sided Jetmentioning

confidence: 96%

Development of a two-sided relativistic jet in Cygnus X-3

Martı́

Paredes

Peracaula

2001

A&A

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Abstract. We present multi-epoch radio maps of the microquasar Cygnus X-3 obtained with the Very Large Array (VLA). The observations were carried out as a Target-of-Opportunity (ToO) project triggered by a series of strong (>5 Jy) radio outbursts in September 2000. We find that Cygnus X-3 was well resolved and clearly elongated in the North-South direction at the VLA resolution in the weeks after the triggering events. In particular, the VLA map from our final epoch of observation perfectly shows the development of a two-sided radio jet extending over ∼0.05 pc scales. We interpret both the proper motion and the brightness asymmetry between the jet components in the framework of special relativity effects. Assuming a distance of 10 kpc, the true jet velocity that we derive is close to 0.5c with a large angle with the line of sight. The possible connection between the VLA bipolar jets and the elongated one-sided structures observed at milli-arcsecond angular scales is also discussed.

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“…During these outbursts, which occur mainly when the source is in the SS, and last several days, Cygnus X-3 reveals the presence of collimated relativistic jets (e.g., Martí et al 2001;Mioduszewski et al 2001;Geldzahler et al 1983;Miller-Jones et al 2004). Thus, Cygnus X-3 has been classified as a microquasar.…”

Section: Introductionmentioning

confidence: 99%

MAGIC CONSTRAINTS ON Γ-Ray EMISSION FROM CYGNUS X-3

Aleksić

Antonelli

Antoranz

et al. 2010

ApJ

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Cygnus X-3 is a microquasar consisting of an accreting compact object orbiting around a Wolf-Rayet star. It has been detected at radio frequencies and up to high-energy γ rays (above 100 MeV). However, many models also predict a very high energy (VHE) emission (above hundreds of GeV) when the source displays relativistic persistent jets or transient ejections. Therefore, detecting such emission would improve the understanding of the jet physics. The imaging atmospheric Cherenkov telescope MAGIC observed Cygnus X-3 for about 70 hr between 2006 March 843 844 ALEKSIĆ ET AL.Vol. 721and 2009 August in different X-ray/radio spectral states and also during a period of enhanced γ -ray emission. MAGIC found no evidence for a VHE signal from the direction of the microquasar. An upper limit to the integral flux for energies higher than 250 GeV has been set to 2.2 × 10 −12 photons cm −2 s −1 (95% confidence level). This is the best limit so far to the VHE emission from this source. The non-detection of a VHE signal during the period of activity in the high-energy band sheds light on the location of the possible VHE radiation favoring the emission from the innermost region of the jets, where absorption is significant. The current and future generations of Cherenkov telescopes may detect a signal under precise spectral conditions.

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The 1982 September radio outburst of Cygnus X-3 - Evidence for jetlike emission expanding at not less than about 0.35 C

Cited by 57 publications

References 0 publications

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

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

Development of a two-sided relativistic jet in Cygnus X-3

MAGIC CONSTRAINTS ON Γ-Ray EMISSION FROM CYGNUS X-3

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