High-resolution spectroscopy of the SMC eclipsing binary HD 5980: the HeII lambda 4686 emission line

Details High-resolution spectroscopy of the SMC eclipsing binary HD 5980: the HeII lambda 4686 emission line High-resolution spectroscopy of the SMC eclipsing binary HD 5980: the HeII lambda 4686 emission line

Sep 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...361..231b&link_type=abstract

Astronomy and Astrophysics, v.361, p.231-239 (2000)

Astronomy and Astrophysics

Astrophysics

5

Line Profiles, Techniques: Spectroscopic, Stars: Binaries: Eclipsing, Stars: Individual: Hd 5980, Galaxies: Magellanic Clouds

Scientific paper

During 25 nights distributed between September 1996 and September 1997, a programme of intensive spectroscopy of the SMC WR binary HD 5980 was conducted, providing a series of 116 high-resolution (R = 60 000) profiles of the HeII lambda 4686 emission line. These observations were complemented with 9 additional spectra obtained: 5 in October-November 1998 and 4 in January 1999, with a resolving power of R = 48 000. This observational material has allowed to investigate, as a function of the orbital phase, the variations of the line equivalent width, of the full line width at half-maximum, and of the line radial velocity, over many different orbits. The discovery, on one night, of a profile oscillation at the red side of the emission, on a timescale of ~ 7 hours, is reported. Though revealing a rather complex phase-dependent behaviour of the HeII lambda 4686 line, the analysis of the present data still favours the hypothesis that in HD 5980 this highly variable emission feature does not characterize a genuine WR star, but arises instead in a wind-wind collision shock zone. Based on observations carried out at ESO, La Silla, Chile

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