Wolf-Rayet stars in the Magellanic Clouds. II - The peculiar eclipsing binary HD 5980 in the SMC

Details Wolf-Rayet stars in the Magellanic Clouds. II - The peculiar eclipsing binary HD 5980 in the SMC Wolf-Rayet stars in the Magellanic Clouds. II - The peculiar eclipsing binary HD 5980 in the SMC

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...257..116b&link_type=abstract

Astrophysical Journal, Part 1, vol. 257, June 1, 1982, p. 116-124. Research supported by the Natural Sciences and Engineering R

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46

Eclipsing Binary Stars, Magellanic Clouds, O Stars, Peculiar Stars, Stellar Spectrophotometry, Wolf-Rayet Stars, Absorption Spectra, Eccentric Orbits, Emission Spectra, Helium Ions, Light (Visible Radiation), Line Spectra, Periodic Variations, Radial Velocity, Stellar Envelopes, Stellar Mass

Scientific paper

Over seventy spectra from two observatories are combined to study this eclipsing W-R binary, which has components of type WN4 + O7 I:. The orbital period, P = 19.266 d + or - 0.003 d, and the high eccentricity, e = 0.49 + or - 0.10, are confirmed. The width of the strongest optical emission line, He II 4686, decreases by at least a factor of two at each eclipse. This is tentatively interpreted in terms of phase-dependent variations of a combination of emission from the W-R envelope as a whole, a hot localized region in the W-R envelope, and the O component wind. Radial velocity variations of He II 4686 probably do not reflect the true W-R orbit; assumption of a mass ratio similar to those observed for other early-WN binaries, along with the more reliable absorption-line orbit of the O component, yield minimum masses of eight solar masses for the W-R star and 27 solar masses for the O-star.

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