B(e)-supergiants of the Magellanic Clouds

Details B(e)-supergiants of the Magellanic Clouds B(e)-supergiants of the Magellanic Clouds

Jul 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...163..119z&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 163, no. 1-2, July 1986, p. 119-134.

Astronomy and Astrophysics

Astrophysics

154

B Stars, Magellanic Clouds, Stellar Spectra, Supergiant Stars, Astronomical Photometry, Balmer Series, Emission Spectra, H Alpha Line, Hertzsprung-Russell Diagram, Iue, Radial Velocity, Spectral Energy Distribution

Scientific paper

Spectroscopic and photometric observations at the satellite UV, visual, and infrared wavelengths of 8 Magellanic Clouds dusty B[e]-supergiants are discussed. In spite of their high luminosity these stars show little or no photometric or spectroscopic variations. Apart from R 66 (B8 Ia) all stars are early B supergiants. The peculiar emission line spectra appear to be a consequence of unique wind characteristics. A two component stellar wind model, comprising a slow, dense, cool equatorial wind and a normal radiation driven wind in the polar region, can account for the observations. It is concluded that the known B[e]-stars of the Magellanic Clouds are massive (30 ⪉ M ⪉ 80 M_sun;) post-main sequence objects where stellar rotation plays an important role for the mass loss.

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