A giant radio flare from Cygnus X-3 with associated γ-ray emission

Corbel, S.; Dubus, G.; Tomsick, John A.; Szostek, A.; Corbet, R. H. D.; Miller-Jones, J. C. A.; Richards, J. L.; Pooley, G. G.; Трушкин, С. А.; Dubois, R.; Hill, A. B.; Kerr, M.; Max-Moerbeck, W.; Readhead, A. C. S.; Bodaghee, A.; Tudose, V.; Parent, D.; Wilms, J.; Pottschmidt, K.

doi:10.1111/j.1365-2966.2012.20517.x

Cited by 89 publications

(94 citation statements)

References 53 publications

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“…In both cases the GeV emission is most likely produced by inverse Compton scattering on stellar photons (Fermi LAT Collaboration et al 2009;Dubus et al 2010). However, contrarily to Cygnus X-1, the conditions required to detect gamma rays from Cygnus X-3 are that the source is in the SS and showing significant emission (0.2-0.4 Jy) with rapid variations in the radio flux from the radio jets (Corbel et al 2012). The latter is probably related to strong shocks (probably due to discrete jet ejections) occurring when the source undergoes state transitions in and out of the ultra-SS.…”

Section: Discussionmentioning

confidence: 99%

“…So far, the only microquasar (i.e. XRB displaying relativistic jets) firmly detected at high energies (> 100 MeV) is Cygnus X-3 (Tavani et al 2009;Fermi LAT Collaboration et al 2009) and its gamma-ray emission is related to the formation/existence of the radio jets (Piano et al 2012;Corbel et al 2012). However Malyshev et al (2013) showed there is a 4σ-level evidence of gamma-ray signal for Cygnus X-1, above 100 MeV, in 3.8 yr of Fermi-LAT data, only when the source is in the HS.…”

Section: Introductionmentioning

confidence: 99%

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Gamma rays detected from Cygnus X-1 with likely jet origin

Zanin

Fernández-Barral

Wilhelmi

et al. 2016

A&A

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Aims. Probe the high-energy (>60 MeV) emission from the black hole X-ray binary system, Cygnus X-1, and investigate its origin. Methods. We analysed 7.5 yr of data by Fermi-LAT with the latest Pass 8 software version. Results. We report the detection of a signal at ∼8 σ statistical significance spatially coincident with Cygnus X-1 and a luminosity above 60 MeV of 5.5×10 33 erg s −1 . The signal is correlated with the hard X-ray flux: the source is observed at high energies only during the hard X-ray spectral state, when the source is known to display persistent, relativistic radio emitting jets. The energy spectrum, extending up to ∼20 GeV without any sign of spectral break, is well fitted by a power-law function with a photon index of 2.3±0.2. There is a hint of orbital flux variability, with high-energy emission mostly coming around the superior conjunction. Conclusions. We detected GeV emission from Cygnus X-1 and probed that the emission is most likely associated with the relativistic jets. The evidence of flux orbital variability points to the anisotropic inverse Compton on stellar photons as the mechanism at work, thus constraining the emission region to a distance 10 11 − 10 13 cm from the black hole.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Gamma rays detected from Cygnus X-1 with likely jet origin

Zanin

Fernández-Barral

Wilhelmi

et al. 2016

A&A

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“…This microquasar consists of a Wolf-Rayet star and a compact object (most likely a black hole), and shows frequent and strong flaring activity. The Cyg X-3 multi-wavelength monitoring campaign reported by Corbel et al (2012) shows a sharp transition from a quenched state to a major flare, with an onset estimated at MJD 55641.0±0.5 (i.e. March 21).…”

Section: Data Reductionmentioning

confidence: 99%

The 2.35 year itch of Cygnus OB2 #9

Blomme

Nazé

Volpi

et al. 2013

A&A

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Context. Cyg OB2 #9 is one of a small set of non-thermal radio emitting massive O-star binaries. The non-thermal radiation is due to synchrotron emission in the colliding-wind region. Cyg OB2 #9 has only recently been discovered to be a binary system, and a multi-wavelength campaign was organized to study its 2011 periastron passage. Aims. We want to better determine the parameters of this system and model the wind-wind collision. This will lead to a better understanding of the Fermi mechanism that accelerates electrons up to relativistic speeds in shocks and its occurrence in collidingwind binaries. We report here on the results of the radio observations obtained in the monitoring campaign and present a simple model to interpret the data. Methods. We used the Expanded Very Large Array (EVLA) radio interferometer to obtain 6 cm and 20 cm continuum fluxes during the Cyg OB2 #9 periastron passage in 2011. We introduce a simple model to solve the radiative transfer in the stellar winds and the colliding-wind region, and thus determine the expected behaviour of the radio light curve. Results. The observed radio light curve shows a steep drop in flux sometime before periastron. The fluxes drop to a level that is comparable to the expected free-free emission from the stellar winds, suggesting that the non-thermal emitting region is completely hidden at that time. After periastron passage, the fluxes slowly increase. We use the asymmetry of the light curve to show that the primary has the stronger wind. This is somewhat unexpected if we use the astrophysical parameters based on theoretical calibrations. But it becomes entirely feasible if we take into account that a given spectral type-luminosity class combination covers a range of astrophysical parameters. The colliding-wind region also contributes to the free-free emission, which can help explain the high values of the spectral index seen after periastron passage. Combining our data with older Very Large Array (VLA) data allows us to derive a period P = 860.0 ± 3.7 days for this system. With this period, we update the orbital parameters that were derived in the first paper of this series. Conclusions. A simple model introduced to explain only the radio data already allows some constraints to be put on the parameters of this binary system. Future, more sophisticated, modelling that will also include optical, X-ray, and interferometric information will provide even better constraints.

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“…During 2006-2009 Cyg X-3 showed similar dependencies between soft (RXTE ASM), hard (Swift/BAT) X-rays and radio emission ( [1,6,[8][9][10]). Gamma-ray emission was detected during the flaring states ( [11,12]).…”

Section: Monitoring Program Of Microquasars With the Ratan-600 Telescopementioning

confidence: 94%

The Giant Flares of the Microquasar Cygnus X-3: X-Rays States and Jets

et al. 2017

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Abstract:We report on two giant radio flares of the X-ray binary microquasar Cyg X-3, consisting of a Wolf-Rayet star and probably a black hole. The first flare occurred on 13 September 2016, 2000 days after a previous giant flare in February 2011, as the RATAN-600 radio telescope daily monitoring showed. After 200 days on 1 April 2017, we detected a second giant flare. Both flares are characterized by the increase of the fluxes by almost 2000-times (from 5-10 to 17,000 mJy at 4-11 GHz) during 2-7 days, indicating relativistic bulk motions from the central region of the accretion disk around a black hole. The flaring light curves and spectral evolution of the synchrotron radiation indicate the formation of two relativistic collimated jets from the binaries. Both flares occurred when the source went from hypersoft X-ray states to soft ones, i.e. hard fluxes (Swift/BAT 15-50 keV data) dropped to zero, the soft X-ray fluxes (MAXI 2-10 keV data) staying high, and then later, the binary came back to a hard state. Both similar giant flares indicated the unchanged mechanism of the jets' formation in Cyg X-3, probably in conditions of strong stellar wind and powerful accretion onto a black hole.

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A giant radio flare from Cygnus X-3 with associated γ-ray emission

Cited by 89 publications

References 53 publications

Gamma rays detected from Cygnus X-1 with likely jet origin

Gamma rays detected from Cygnus X-1 with likely jet origin

The 2.35 year itch of Cygnus OB2 #9

The Giant Flares of the Microquasar Cygnus X-3: X-Rays States and Jets

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