Line formation in winds with enhanced equatorial mass-loss rates and its application to the Wolf-Rayet star HD 50896

Rumpl, William M.

doi:10.1086/158420

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Optical Depth : DX = -Kpdr1

Introduction1

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1982

1995

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Cited by 21 publications

(2 citation statements)

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“…Information on the velocity structure in WR-winds can be found in Hartmann et al(l9T7), Hartmann (1978) and Rumpl (1980). The change in the optical depth due to the second acceleration at about ten stel lar radii is less than 0.01 so that we neglected this peculiarity.…”

Section: Optical Depth : DX = -Kpdrmentioning

confidence: 99%

Corrections for Hydrostatic Atmospheric Models: Radii and Effective Temperatures of Wolf Rayet Stars

Loore¹,

Hellings²,

Lamers

1982

Symp. - Int. Astron. Union

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Section: Optical Depth : DX = -Kpdrmentioning

confidence: 99%

Corrections for Hydrostatic Atmospheric Models: Radii and Effective Temperatures of Wolf Rayet Stars

Loore¹,

Hellings²,

Lamers

1982

Symp. - Int. Astron. Union

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“…Such a model has been suggested by Stella, White & Rosner (1986), in a scenario in which the neutron star is spun up by the accretion of angular momentum until centrifugal inhibition of accretion occurs and the system is X-ray quiet. Alternative explanations for the variabiity in HD 50896 and other WRs with similar characteristics include the presence of a disk (Rumpl 1980;Schulte-Ladbeck et al 1991), rotating jet-like structures (Matthews et al 1992), and intrinsic wind instabilities (St-Louis et al 1993). Thus, observational evidence for the existence of WR+cc systems is as yet inconclusive.…”

Section: Introductionmentioning

confidence: 99%

Line profile variations in WR + collapsed companion systems

Koenigsberger¹

1995

Symp. - Int. Astron. Union

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The existence of Wolf-Rayet binary systems containing a collapsed companion is predicted on evolutionary grounds. However, because of the absence of strong X-ray emission and the difficulty in obtaining consistent periodicities from the observed variations, none of the “classical” WR stars has been shown to be a WR+cc system. A discussion is presented of the line-profile variations which are predicted to occur on orbital timescales due to the interaction of the WR wind with the cc. We note the importance of numerical simulations of the flow structure of the WR wind in the vicinity of a collapsed companion for deriving diagnostic tools for the presence of a cc in a WR system.

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Stellar Chromospheres, Coronae, and Winds

Cassinelli

MacGregor

1986

Physics of the Sun

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Line formation in winds with enhanced equatorial mass-loss rates and its application to the Wolf-Rayet star HD 50896

Cited by 21 publications

References 0 publications

Corrections for Hydrostatic Atmospheric Models: Radii and Effective Temperatures of Wolf Rayet Stars

Corrections for Hydrostatic Atmospheric Models: Radii and Effective Temperatures of Wolf Rayet Stars

Line profile variations in WR + collapsed companion systems

Stellar Chromospheres, Coronae, and Winds

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