Cygnus X-3 as a benchmark for fundamental properties of Wolf-Rayet stars

Cherepashchuk, A. M.; Moffat, A. F. J.

doi:10.1086/187273

Cited by 50 publications

(31 citation statements)

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“…Minimization of the residual functional, η, taking into account the constraints (8) was undertaken using an efficient method of conjugate gradient projection (Goncharsky et al, 1985).…”

Section: Methods Of the Light Curve Solutionmentioning

confidence: 99%

“…A very important theorem was proved by Tikhonov (1943): if we select a compact set of functions using physical "a priori" information about the function of interest, an initially ill-posed problem becomes a well-posed one. Efficient algorithms of solving ill-posed problems on compact sets of functions were developed by Goncharsky et al (1985). The light curve solution for V444 Cyg was obtained at the following compact sets of functions (see Figure 1):…”

Section: Development Of Kopal's Ideamentioning

confidence: 99%

“…Cyg X-3, a peculiar short-period (P 4 h .8) X-ray binary system (e.g., Cherepashchuk et al, 1996). The optical companion is a WN3-7 star (van Kerkwijk et al, 1992), it is a massive WR star with L bol 3 · 10 39 erg/s (van Kerkwijk et al, 1992;Cherepashchuk and Moffat, 1994). Its very short orbital period, P 4 h .8, implies the separation between the WR and X-ray components a 3.2 − 5.6 R .…”

Section: An Analysis Of Variable Linear Polarization At Different Orbmentioning

confidence: 99%

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Atmospheric Eclipses in Wr+o Binaries: From Kopal and Shapley to Present Days

Черепащук¹

2005

Astrophys Space Sci

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Kopal and Shapley (1946) were the first to suggest to solve an integral equation for interpretation of atmospheric eclipses in WR+O binary systems. In our studies, this idea was developed in two ways: solution of two integral equations; development of efficient methods of solution of ill-posed problems.Application of the new method to the interpretation of the light curve of the WN5+O6 eclipsing binary V444 Cyg allowed us to determine the radius and the temperature of the WN5 star core. Some astrophysical applications of these results are presented.

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“…Minimization of the residual functional, η, taking into account the constraints (8) was undertaken using an efficient method of conjugate gradient projection (Goncharsky et al, 1985).…”

Section: Methods Of the Light Curve Solutionmentioning

confidence: 99%

Section: Development Of Kopal's Ideamentioning

confidence: 99%

Section: An Analysis Of Variable Linear Polarization At Different Orbmentioning

confidence: 99%

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Atmospheric Eclipses in Wr+o Binaries: From Kopal and Shapley to Present Days

Черепащук¹

2005

Astrophys Space Sci

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“…radiation fields of the accretion disk and the corona (see the stellar parameters in the last four lines of Table 2 which were taken from Cherepashchuk & Moffat 1994). The orbital phase considered was φ b = 0.9, near the superior conjunction (Aleksic et al 2010), as in Cyg X-1.…”

Section: Application To Cygnus X-3mentioning

confidence: 99%

A magnetic reconnection model for explaining the multiwavelength emission of the microquasars Cyg X-1 and Cyg X-3

Khiali

Pino

Valle

2015

Monthly Notices of the Royal Astronomical Society

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Recent studies have indicated that cosmic ray acceleration by a first-order Fermi process in magnetic reconnection current sheets can be efficient enough in the surrounds of compact sources. In this work, we discuss this acceleration mechanism operating in the core region of galactic black hole binaries (or microquasars) and show the conditions under which this can be more efficient than shock acceleration. In addition, we compare the corresponding acceleration rate with the relevant radiative loss rates obtaining the possible energy cut-off of the accelerated particles and also compute the expected spectral energy distribution (SED) for two sources of this class, namely Cygnus X-1 and Cygnus X-3, considering both leptonic and hadronic processes. The derived SEDs are comparable to the observed ones in the low and high energy ranges. Our results suggest that hadronic non-thermal emission due to photo-meson production may produce the very high energy gamma-rays in these microquasars.

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“…The distance to Cyg X-3 is ∼7 or ∼9 kpc, depending on the method used (Predehl et al 2000;Ling et al 2009). It is also uncertain whether the compact object is a black hole (e.g., Cherepashchuk & Moffat 1994) or neutron star (e.g., Stark & Saia 2003).…”

Section: Introductionmentioning

confidence: 99%

The 2010 MAY FLARING EPISODE OF CYGNUS X-3 IN RADIO, X-Rays, AND Γ-Rays

Williams¹,

Tomsick²,

Bodaghee³

et al. 2011

ApJ

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In 2009, Cygnus X-3 (Cyg X-3) became the first microquasar to be detected in the GeV γ -ray regime, via the satellites Fermi and AGILE. The addition of this new band to the observational toolbox holds promise for building a more detailed understanding of the relativistic jets of this and other systems. We present a rich data set of radio, hard and soft X-ray, and γ -ray observations of Cyg X-3 made during a flaring episode in 2010 May. We detect a ∼3 day softening and recovery of the X-ray emission, followed almost immediately by a ∼1 Jy radio flare at 15 GHz, followed by a 4.3σ γ -ray flare (E > 100 MeV) ∼1.5 days later. The radio sampling is sparse, but we use archival data to argue that it is unlikely the γ -ray flare was followed by any significant unobserved radio flares. In this case, the sequencing of the observed events is difficult to explain in a model in which the γ -ray emission is due to inverse Compton scattering of the companion star's radiation field. Our observations suggest that other mechanisms may also be responsible for γ -ray emission from Cyg X-3.

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Cygnus X-3 as a benchmark for fundamental properties of Wolf-Rayet stars

Cited by 50 publications

References 0 publications

Atmospheric Eclipses in Wr+o Binaries: From Kopal and Shapley to Present Days

Atmospheric Eclipses in Wr+o Binaries: From Kopal and Shapley to Present Days

A magnetic reconnection model for explaining the multiwavelength emission of the microquasars Cyg X-1 and Cyg X-3

The 2010 MAY FLARING EPISODE OF CYGNUS X-3 IN RADIO, X-Rays, AND Γ-Rays

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