The problem of V444 Cygni

Details The problem of V444 Cygni The problem of V444 Cygni

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...313..358u&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 313, Feb. 1, 1987, p. 358-375.

Astronomy and Astrophysics

Astrophysics

27

Eclipsing Binary Stars, Light Curve, Stellar Orbits, Ultraviolet Spectra, Wolf-Rayet Stars, Emission Spectra, Iue, Line Spectra, O Stars, Stellar Spectrophotometry

Scientific paper

The authors have studied the changes of the spectrum of V444 Cygni (WN5+O6) shown on 13 high-resolution spectrograms obtained with the IUE. Evidence is found for an orbital-phase-dependent "third light" both in line and in continuum wavelengths. A model for the V444 Cygni system consisting of an O star with Teff = 40,000K, R/R_sun; = 10, and a Wolf-Rayet star with Teff = 30,000K, R/R_sun; = 9, will reproduce the energy curve observed from 1300 to 6000 Å. The authors describe a model Wolf-Rayet star possessing large, readily visible, magnetic field-supported plumes which envelop both stars. The emission-line spectrum from these plumes and stellar continuum light scattered by the plumes could explain the observed light curve distortions.

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