The Evolution of Outbursts in Cygnus X-3 at 2.25 and 8.3 GHz

Waltman, E. B.; Ghigo, F. D.; Johnston, K. J.; Foster, Roger S.; Fiedler, Russell; Spencer, J. H.

doi:10.1086/117518

Cited by 70 publications

(84 citation statements)

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“…This sequence of outbursts with different spectral characteristics is also found in Cygnus X-3: Fig. 3b shows GBI observations of Cygnus X-3 (Waltman et al 1995), where a first outburst with almost flat spectrum (α ∼ 0.05) is seen, followed by a minor optically thin flare. Figure 3c displays a first outburst exhibiting an inverted spectrum (α ∼ 0.6) followed by a bursting phase of optically thin emission, as also seen for LS I +61 • 303 in the GBI observations of Fig.…”

Section: Discussionsupporting

confidence: 58%

The broad-band radio spectrum of LS I +61°303 in outburst

Zimmermann

Fuhrmann

Massi

2015

A&A

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Aims. Our aim is to explore the broad-band radio continuum spectrum of LS I +61 • 303 during its outbursts by employing the available set of secondary focus receivers of the Effelsberg 100 m telescope. Methods. The clear periodicity of the system LS I +61 • 303 allowed observations to be scheduled covering the large radio outburst in March-April 2012. We observed LS I +61 • 303 on 14 consecutive days at 2. 6, 4.85, 8.35, 10.45, 14.3, 23, and 32 GHz with a cadence of about 12 h followed by two additional observations several days later. Based on these observations we obtained a total of 24 quasi-simultaneous broad-band radio spectra. Results. During onset, the main flare shows an almost flat broad-band spectrum, most prominently seen on March 27, 2012, wherefor the first time -a flat spectrum (α = 0.00 ± 0.07, S ∝ ν α ) is observed up to 32 GHz (9 mm wavelength). The flare decay phase shows superimposed "sub-flares" with the spectral index oscillating between −0.4 and −0.1 in a quasi-regular fashion. Finally, the spectral index steepens during the decay phase, showing optically thin emission with values α ∼ −0.5 to −0.7. Conclusions. The radio characteristics of LS I +61 • 303 compare well with those of the microquasars XTE J1752-223 and Cygnus X-3. In these systems the flaring phase is actually also composed of a sequence of outbursts with clearly different spectral characteristics: a first outburst with a flat/inverted spectrum followed by a bursting phase of optically thin emission.

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Section: Discussionsupporting

confidence: 58%

The broad-band radio spectrum of LS I +61°303 in outburst

Zimmermann

Fuhrmann

Massi

2015

A&A

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“…The nature of the compact object is not certain, but it is thought to be a black hole due to its spectral resemblance to other black hole XRB systems, such as GRS 1915+105 and XTE J1550−564. In addition, there is no evidence of a neutron star system producing such massive radio outbursts (up to ∼20 Jy, Waltman et al 1995) as observed from Cyg X-3. Cyg X-3 is a unique system in our Galaxy, but (Koljonen et al 2010).…”

Section: Introductionmentioning

confidence: 97%

The disk/jet connection in the enigmatic microquasar Cygnus X-3

Koljonen

Hannikainen

McCollough³

et al. 2010

Proc. IAU

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Abstract. Simultaneous multi-wavelength observations are crucial for understanding the physics of microquasars, especially the accretion disk/jet connection. The enigmatic microquasar Cygnus X-3 exhibits strong, relativistic jet ejection events producing radio flares up to 20 Jy. These events are preceded by a very soft X-ray state with quenched emission in the radio and hard X-ray bands. Recently, GeV flux was observed by the AGILE and Fermi γ-ray observatories during the newly-identified hypersoft state. By using an extensive database of simultaneous multi-wavelength observations gathered from Cygnus X-3 we can form a more unified picture of the nature of the source and show how the recent γ-ray observations fit into it.

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“…The radio emission shows flaring activity (Gregory et al 1972;Watanabe et al 1994;McCollough et al 1999) during which it exhibits radio-jets analogous to those of powerful radio galaxies and quasars (Waltman et al 1995;Fender et al1997). There have been several attempts to connect the radio, X-ray, and infrared variations in the source (Watanabe et al 1994;Fender 1997).…”

Section: Introductionmentioning

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 Evolution of Outbursts in Cygnus X-3 at 2.25 and 8.3 GHz

Cited by 70 publications

References 0 publications

The broad-band radio spectrum of LS I +61°303 in outburst

The broad-band radio spectrum of LS I +61°303 in outburst

The disk/jet connection in the enigmatic microquasar Cygnus X-3

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

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