High-resolution X-ray imaging of the colliding wind shock in WR 147

Pittard, J. M.; Stevens, I. R.; Williams, P. M.; Pollock, A. M. T.; Skinner, Stephen L.; Corcoran, M. F.; Moffat, A. F. J.

doi:10.1051/0004-6361:20020465

Cited by 33 publications

(31 citation statements)

References 41 publications

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“…Statistical tests reveal the X-ray emission to be extended (FWHM~0.8, roughly double that of the PSF). We also find that models of the wind collision zone are in rough quantitative agreement, and in particular predict a FWHM consistent with that measured (Pittard et al 2002). A deeper observation is needed to accurately measure the spatial extension, to align the X-ray and optical/radio frames, and to determine the level of contamination from the stars.…”

Section: Introductionsupporting

confidence: 60%

High-resolution X-ray imaging of the colliding wind shock in WR 147 (WN8(h)+B0.5V)

Pittard

Stevens

Williams

et al. 2003

Symp. - Int. Astron. Union

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Abstract. We present the results of a high-resolution Chandra X-ray image of the Wolf-Rayet binary system WR 147, which consists of a WN8 star and an early-type companion located ff.'6 to its north. The image provides the first direct evidence for spatially extended X-ray emission in an early-type binary system, and shows that the emission peaks north-of the WN8 star and close to the position of the radio bow shock. Simulated X-ray images of the wind-wind collision have a FWHM consistent with the data, but cannot account for the full spatial extension, unless emission from the stars is also included.

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Section: Introductionsupporting

confidence: 60%

High-resolution X-ray imaging of the colliding wind shock in WR 147 (WN8(h)+B0.5V)

Pittard

Stevens

Williams

et al. 2003

Symp. - Int. Astron. Union

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“…We note that WR 147 is known as a colliding-wind binary that has been spatially resolved (Williams et al 1997;Skinner et al 1999), with a separation on the sky large enough for the wind-wind collision zone between the stars to be resolved at near-infrared and radio (Williams et al 1997), and X-ray energies (Pittard et al 2002). The spectral energy distribution of WR 147 in the 0.5 µm to 2 mm wavelength range (including all components) shown by Williams et al (1997) is dominated by the free-free emission from the stellar wind of the WN8 star; in the 2 to 10 µm range these authors find α = 1.0, in good agreement with our ISOPHOT-S measurement (when dereddened with the Lutz et al 1996 law); and in the mid-infrared to radio range they find α = 0.66.…”

Section: Resultsmentioning

confidence: 99%

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

Koch-Miramond

Ábrahám

Fuchs

et al. 2002

A&A

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Abstract. We present mid-infrared spectrophotometric results obtained with the ISO on the peculiar X-ray binary Cygnus X-3 in quiescence, at orbital phases 0.83 to 1.04. The 2.4-12 µm continuum radiation observed with ISOPHOT-S can be explained by thermal free-free emission in an expanding wind with, above 6.5 µm, a possible additional black-body component with temperature T ∼ 250 K and radius R ∼ 5000 R at 10 kpc, likely due to thermal emission by circumstellar dust. The observed brightness and continuum spectrum closely match that of the Wolf-Rayet star WR 147, a WN8 +B0.5 binary system, when rescaled at the same 10 kpc distance as Cygnus X-3. A rough mass loss estimate assuming a WN wind gives ∼1.2 × 10 −4 M yr −1 . A line at ∼4.3 µm with a more than 4.3 σ detection level, and with a dereddened flux of 126 mJy, is interpreted as the expected He I 3p-3s line at 4.295 µm, a prominent line in the WR 147 spectrum. These results are consistent with a Wolf-Rayet-like companion to the compact object in Cyg X-3 of WN8 type, a later type than suggested by earlier works.

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“…Interestingly, WR 147 is also the first early-type system where high resolution Chandra ACIS-I observations provided evidence for a spatially extended X-ray emission. The X-rays are found to peak close to the position of the radio bow shock (Pittard et al 2002).…”

Section: Non-thermal Radio Emission From Early-type Starsmentioning

confidence: 90%

Non-Thermal Emission from Early-Type Binaries

Rauw

2004

Cosmic Gamma-Ray Sources

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In this chapter, I review the properties of high-energy particles in the stellar winds of hot early-type stars. Relativistic electrons are responsible for the synchrotron radio emission observed from a subsample of these stars. Most of the objects in the latter category are found to be binaries and the collision between the stellar winds of the binary components is thought to play a crucial role in the acceleration of the relativistic electrons. The interplay between these high-energy electrons and the intense stellar radiation field could produce a substantial nonthermal emission at X-ray and γ-ray energies through inverse Compton scattering. Other mechanisms, such as π 0 decay might also contribute to the production of non-thermal emission from hot stars. These various effects could possibly account for some of the yet unidentified EGRET sources found to be correlated with OB associations in our Galaxy. Finally, I review recent results from XMM-Newton observations and discuss the prospects of forthcoming γ-ray observations with INTEGRAL and GLAST.

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High-resolution X-ray imaging of the colliding wind shock in WR 147

Cited by 33 publications

References 41 publications

High-resolution X-ray imaging of the colliding wind shock in WR 147 (WN8(h)+B0.5V)

High-resolution X-ray imaging of the colliding wind shock in WR 147 (WN8(h)+B0.5V)

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

Non-Thermal Emission from Early-Type Binaries

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