The Wolf‐Rayet Binary V444 Cygni Under the Spectroscopic Microscope. II. Physical Parameters of the Wolf‐Rayet Wind and the Zone of Wind Collision

Марченко, С. В.; Moffat, A. F. J.; Cardona, O.; Echevarría, J.; Hervieux, Yannick

doi:10.1086/304435

Cited by 35 publications

(44 citation statements)

References 40 publications

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“…• (Marchenko et al 1997). Additionally, in their 1997 analysis, Marchenko et al suggested that one of the bow shock arms crosses our line of sight near phase 0.73.…”

mentioning

confidence: 73%

“…Third and most importantly, Kasen et al (2004) considered a distributed emission source, with photon packets arising from throughout their model atmosphere to simulate the energy deposition from decaying 56 Ni and 56 Co into the supernova ejecta. This distributed emission is also a good representation of the line-emitting shells surrounding the WN star in V444 Cyg (Marchenko et al 1997). Kasen et al (2004) oriented their models such that all the polarization variations occurred in one Stokes parameter.…”

Section: Optical Polarimetrymentioning

confidence: 96%

“…Photospheric absorption in the O star is an important source of line profile variations observed in total light (Marchenko et al 1997;Flores et al 2001). If we do not correct for this unpolarized absorption we risk removing too much continuum polarization from our observations.…”

Section: Optical Polarimetrymentioning

confidence: 99%

“…(2); this reduces the value of F c so as to produce a specified absorption equivalent width, as detailed by Hoffman et al (1998). Marchenko et al (1997) an EW of 0.25 Å. While we do not know the EW of the NV doublet that is also blended with the HeII λ4686 line, we assumed an underlying unpolarized absorption component using a total EW of 2 Å.…”

Section: Optical Polarimetrymentioning

confidence: 99%

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V444 Cygni X-ray and polarimetric variability: Radiative and Coriolis forces shape the wind collision region

Lomax

Nazé

Hoffman

et al. 2014

A&A

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We present results from a study of the eclipsing, colliding-wind binary V444 Cyg that uses a combination of X-ray and optical spectropolarimetric methods to describe the 3D nature of the shock and wind structure within the system. We have created the most complete X-ray light curve of V444 Cyg to date using 40 ks of new data from Swift, and 200 ks of new and archived XMM-Newton observations. In addition, we have characterized the intrinsic, polarimetric phase-dependent behavior of the strongest optical emission lines using data obtained with the University of Wisconsin's Half-Wave Spectropolarimeter. We have detected evidence of the Coriolis distortion of the wind-wind collision in the X-ray regime, which manifests itself through asymmetric behavior around the eclipses in the system's X-ray light curves. The large opening angle of the X-ray emitting region, as well as its location (i.e. the WN wind does not collide with the O star, but rather its wind) are evidence of radiative braking/inhibition occurring within the system. Additionally, the polarimetric results show evidence of the cavity the wind-wind collision region carves out of the Wolf-Rayet star's wind.

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“…• (Marchenko et al 1997). Additionally, in their 1997 analysis, Marchenko et al suggested that one of the bow shock arms crosses our line of sight near phase 0.73.…”

mentioning

confidence: 73%

Section: Optical Polarimetrymentioning

confidence: 96%

Section: Optical Polarimetrymentioning

confidence: 99%

Section: Optical Polarimetrymentioning

confidence: 99%

See 2 more Smart Citations

V444 Cygni X-ray and polarimetric variability: Radiative and Coriolis forces shape the wind collision region

Lomax

Nazé

Hoffman

et al. 2014

A&A

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“…V444Cygni (WR139, WN5+06III-V, P=4.21 d, e=O.04) Colliding wind effects in V444 Cygni have been well documented in the UV and optical (Shore & Brown 1988;Marchenko et al 1997;Flores et al 2001). It was expected that V444 Cyg would exhibit colliding wind X-ray emission at a level Lx~10 34 -35 erg s"!…”

Section: Colliding Wind X-ray Emissionmentioning

confidence: 98%

X-ray observations of massive colliding wind binaries

Corcoran

2003

Symp. - Int. Astron. Union

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Abstract. Masslve stars in binary systems can generate X-ray emission in the region between the two stars where stellar winds collide. Colliding wind X-ray emission acts as an in-situ probe of important wind parameters like massloss rates, chemical abundances, wind velocities, and possibly magnetic field strengths. Variations in observed colliding-wind X-ray emission can be produced by the changing line-of-sight to the colliding wind region as the stars move in orbit and/or the changing emission measure of the shocked gas in the wind collision zone produced if the separations between the two stars change. X-ray variability depends on the wind and orbital parameters and so can in principal allow the direct measurement of mass functions even for low inclination systems and provide a connection between the stellar and wind parameters. X-rayemission from colliding wind systems can thus be used to refine our understanding of the evolutionary state of massive stars and to help test evolutionary models. We discuss recent advances in defining the X-ray spectral and temporal signatures of colliding wind X-ray emission using ROSAT~ASCA, RXTE~Chandra and XMM-Newton data.

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Wind variations of wolf-rayet stars

Moffat

Variable and Non-Spherical Stellar Winds in Luminous Hot Stars

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The Wolf‐Rayet Binary V444 Cygni Under the Spectroscopic Microscope. II. Physical Parameters of the Wolf‐Rayet Wind and the Zone of Wind Collision

Cited by 35 publications

References 40 publications

V444 Cygni X-ray and polarimetric variability: Radiative and Coriolis forces shape the wind collision region

V444 Cygni X-ray and polarimetric variability: Radiative and Coriolis forces shape the wind collision region

X-ray observations of massive colliding wind binaries

Wind variations of wolf-rayet stars

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