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

Трушкин, С. А.; McCollough, Michael L.; Nizhelskij, N. A.; Цыбулев, П. Г.

doi:10.3390/galaxies5040086

Cited by 15 publications

(8 citation statements)

References 18 publications

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“…We detected two giant flares from Cyg X-3 in September 2016 and in April 2017 at 1.3-30 GHz. We discuss the properties of these flares in the paper of the Proceedings of [4].…”

Section: Microquasars Studies With the Ratan-600 Telescopementioning

confidence: 99%

The Jets of Microquasars during Giant Flares and Quiet State

et al. 2017

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Abstract:We report on the radio properties of jets of the following microquasars, as determined from daily multi-frequency monitoring observations with the RATAN-600 radio telescope during 2010-2017: V404 Cyg, SS433, Cyg X-1, GRS1915+105 and LSI+61 • 303. We have detected many giant flares from SS433, a powerful flare from V404 Cyg in June 2015, an active state of Cyg X-1 in 2017 and fifty periodic flares from LSI+61 • 303. We describe the properties of massive ejections based on multi-band (radio, X-ray and γ-ray) studies. The general properties of the light curves are closely connected with the processes of jet formation in microquasars.Keywords: stars; X-ray binary; black hole; microquasars; radio emission; X-ray emission; relativistic jets; synchrotron radiation Microquasars Studies with the RATAN-600 TelescopeThe bright microquasars GRS1915+105, SS433, Cyg X-1, Cyg X-3, LSI+61 • 303 and LS5039 are well-known X-ray binaries (XRBs) with relativistic jets, detected directly in the VLBI mapping. The radio emission of XRBs is mostly a variable synchrotron radiation from these jets, formed as a mass of ejections from central regions of an accretion disk within an intensive wind of the optical star. The inner shock waves in relativistic jets are the main generator of the relativistic electrons [1]. We have carried out a long-term monitoring of XRBs in almost daily measurements with RATAN-600 at 1.3-30 GHz during the last seven years [2,3]. During 52 orbital periods (P 1 = 26.5 d) we studied the super-orbital modulation (P 2 = 1667 d) of the flaring radio emission from LSI+61 • 303. The mean orbital light curves (usually for ten orbits) depend strongly on a phase P 2 . We detected two giant flares from Cyg X-3 in September 2016 and in April 2017 at 1.3-30 GHz. We discuss the properties of these flares in the paper of the Proceedings of [4]. Results V404 CygV404 Cygni is a low-mass XRB consisting of a black hole of mass 9.0 M , accreting matter from a low-mass (<1 M ), late-type companion star. The orbital period P 1 = 6.5 d is the longest of all known black hole XRBs. V404 Cyg is the closest microquasar, d = 2.39 kpc [5]. We observed V404 Cyg in June 2015 [6] and have detected the bright flare [7] simultaneously with the huge X-ray flare (40 Crabs at 15-50 keV, [8]) at MJD57198.933 (Figure 1). This flare had the characteristic synchrotron spectrum with a low-frequency turn-over. This is probably due to a synchrotron self-absorption or an absorption due to thermal electrons mixed with the relativistic ones [9]. During four days, the flaring flux decreased with time as a power-law: S ∝ t −1.5 .

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“…We detected two giant flares from Cyg X-3 in September 2016 and in April 2017 at 1.3-30 GHz. We discuss the properties of these flares in the paper of the Proceedings of [4].…”

Section: Microquasars Studies With the Ratan-600 Telescopementioning

confidence: 99%

The Jets of Microquasars during Giant Flares and Quiet State

et al. 2017

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“…The uv photons would be up-scattered into 𝛾 rays (Piano et al 2012). Recent results from Fermi-LAT (Trushkin et al 2017) and AGILE (Piano et al 2021a,b) 𝛾 ray satellites show 𝛾 emission during minor flaring in the radio when just before the quenched state and also at the onset of major flaring at the end of the quenched state. Koljonen et al (2018) suggest this might arise from shocks in the jet, but our results indicate that the 𝛾 ray emission could also be from IC interactions of the high energy electrons responsible for the radio synchrotron emission at the injection phase of the plasmon or jet evolution.…”

Section: Expanding Plasmon Modelmentioning

confidence: 97%

Major and Minor Flares on Cygnus X-3 Revisited

Spencer,

Garrett,

Bray

et al. 2022

Preprint

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Intense flares at cm-wavelengths reaching levels of tens of Jy have been observed from Cygnus X-3 for many years. This active high mass X-ray binary also has periods of quenching before major outbursts, and has minor flares at levels of a few hundred mJy. In this paper we show that the minor flares have much shorter rise times and durations suggesting more rapid expansion of the synchrotron radiation emitting material than in the strong flares. They also appear closer to the binary, whereas the large flares form a more developed jet. Calculations of physical conditions show that the minor out-bursts have lower minimum power but have larger magnetic fields and energy densities than the major flares. Minor flares can occur while a major flare is in progress, suggesting an indirect coupling between them. The spectral evolution of the minor flares can be explained by either an expanding synchrotron source or a shock model. The possibility that there is a brightening zone as in SS433 is explored.

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“…Cygnus is the most radio luminous HMXB in the Galaxy (Trushkin et al 2017;Egron et al 2017;2021 and references therein). Following the same procedure as for Cygnus X-1, from 1550 measurements of the Cygnus X-3 fluxes with GBI it is estimated a mean observed flux of 350 mJy at 21cm.…”

Section: Vi7 Highly Variable Radio Luminous Bh-hmxb-mqs (Rlbh-hmxb-mqs)mentioning

confidence: 99%