A 2.4–12 <i>μ</i>m spectrophotometric study with ISO of Cygnus X-3 in quiescence

Koch-Miramond, L.; Ábrahám, P.; Fuchs, Y.; Bonnet‐Bidaud, J. M.; Claret, A.

doi:10.1051/0004-6361:20021273

Cited by 23 publications

(15 citation statements)

References 32 publications

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“…In both the cases, the radio emission is flat or inverted. The IR emission during radio plateaux in GRS 1915+105 (Fuchs, Mirabel, & Claret 2003;) is closer to the IR emission in Cyg X-3 where wind from the companion always envelops the compact object (Ogley, Burnell, & Fender 2001;Koch-Miramond et al 2002).…”

Section: Resultsmentioning

confidence: 77%

Connection between the Accretion Disk and Superluminal Radio Jets and the Role of the Radio Plateau State in GRS 1915+105

Yadav¹

2006

ApJ

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We investigate the association between the accretion disk during radio plateau state and the following superluminal relativistic radio jets with peak intensity varies from 200 mJy to 1000 mJy observed over a period of five years and present the evidences of direct accretion disc-jet connection in microquasar GRS 1915+105 . We have analysed RXTE PCA/HEXTE X-ray data and have found that the accretion rate,ṁ accr , as inferred from the X-ray flux, is very high during the radio plateaux. We suggest that the accretion disk during the radio plateaux always associated with radiation-driven wind which is manifested in the form of enhanced absorption column density for X-ray and the depleted IR emission. We find that the wind density increases with the accretion disk luminosity during the radio plateaux. The wind density is similar to the density of the warm absorber proposed in extragalactic AGNs and Quasars. We suggest a simple model for the origin of superluminal relativistic jets. Finally, We discuss the implications of this work for galactic microquasars and the extragalactic AGNs and Quasars.

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Section: Resultsmentioning

confidence: 77%

Connection between the Accretion Disk and Superluminal Radio Jets and the Role of the Radio Plateau State in GRS 1915+105

Yadav¹

2006

ApJ

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“…All estimates except one assume spherical symmetry. Note that deviations from spherical symmetry will most probably result in a higher mass-loss rate in the estimates from time delays (Waltman et al 1996;Miller-Jones et al 2005), whereas deviations from spherical symmetry in the other cases will result in a lower effective mass-loss rate from the system (see, e.g., Koch-Miramond et al 2002).…”

Section: Mass-loss Ratementioning

confidence: 99%

Cygnus X-3 and the problem of the missing Wolf-Rayet X-ray binaries

Lommen¹,

Yungelson

Heuvel³

et al. 2005

A&A

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Cygnus X-3 is a strong X-ray source (L X ≈ 10 38 erg s −1 ) which is thought to consist of a compact object accreting matter from a helium star. We analytically find that the estimated ranges of mass-loss rate and orbital-period derivative for Cyg X-3 are consistent with two models: i) the system is detached and the mass loss from the system comes from the stellar wind of a massive helium star, of which only a fraction that allows for the observed X-ray luminosity is accreted, or ii) the system is semidetached and a Roche-lobe-overflowing low-or moderate-mass helium donor transfers mass to the compact object, followed by ejection of its excess over the Eddington rate from the system. These analytical results appear to be consistent with evolutionary calculations. By means of population synthesis we find that currently in the Galaxy there may exist ∼1 X-ray binary with a black hole that accretes from a > ∼ 7 M Wolf-Rayet star and ∼1 X-ray binary in which a neutron star accretes matter from a Roche-lobe-overflowing helium star with mass < ∼ 1.5 M . Cyg X-3 is probably one of these systems.

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“…Discovered by Giacconi et al (1967) at the dawn of X-ray astronomy, Cygnus X-3 (Cyg X-3) is a rare high-mass X-ray binary consisting of a compact object wind-fed by a Wolf-Rayet star (van Kerkwijk et al 1996;Fender et al 1999;Koch-Miramond et al 2002). The nature of the compact object is still uncertain, but a black hole seems to be favored considering X-ray and radio emissions (Hjalmarsdotter et al 2009;Shrader et al 2010, and references therein).…”

Section: Introductionmentioning

confidence: 99%

Single-dish and VLBI observations of Cygnus X-3 during the 2016 giant flare episode

Egron

Pellizzoni

Giroletti

et al. 2017

Monthly Notices of the Royal Astronomical Society

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In September 2016, the microquasar Cygnus X-3 underwent a giant radio flare, which was monitored for 6 days with the Medicina Radio Astronomical Station and the Sardinia Radio Telescope. Long observations were performed in order to follow the evolution of the flare on a hourly scale, covering six frequency ranges from 1.5 GHz to 25.6 GHz. The radio emission reached a maximum of 13.2 ± 0.7 Jy at 7.2 GHz and 10 ± 1 Jy at 18.6 GHz. Rapid flux variations were observed at high radio frequencies at the peak of the flare, together with rapid evolution of the spectral index: α steepened from 0.3 to 0.6 (with S ν ∝ ν −α ) within 5 hours. This is the first time that such fast variations are observed, giving support to the evolution from optically thick to optically thin plasmons in expansion moving outward from the core. Based on the Italian network (Noto, Medicina and SRT) and extended to the European antennas (Torun, Yebes, Onsala), VLBI observations were triggered at 22 GHz on five different occasions, four times prior to the giant flare, and once during its decay phase. Flux variations of 2-hour duration were recorded during the first session. They correspond to a mini-flare that occurred close to the core ten days before the onset of the giant flare. From the latest VLBI observation we infer that four days after the flare peak the jet emission was extended over 30 mas.

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A 2.4–12 μm spectrophotometric study with ISO of Cygnus X-3 in quiescence

Cited by 23 publications

References 32 publications

Connection between the Accretion Disk and Superluminal Radio Jets and the Role of the Radio Plateau State in GRS 1915+105

Connection between the Accretion Disk and Superluminal Radio Jets and the Role of the Radio Plateau State in GRS 1915+105

Cygnus X-3 and the problem of the missing Wolf-Rayet X-ray binaries

Single-dish and VLBI observations of Cygnus X-3 during the 2016 giant flare episode

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