Discovery of a low mass B[e] supergiant in the SMC.

Details Discovery of a low mass B[e] supergiant in the SMC. Discovery of a low mass B[e] supergiant in the SMC.

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989msngr..58...37h&link_type=abstract

The Messenger, vol. 58, p. 37-40

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Magellanic Clouds: B Supergiants, Spectra: B Supergiants, Photometry: B Supergiants

Scientific paper

Peculiar emission-line B supergiants are a group of early-type stars with the following typical characteristics: (a) strong Balmer emission lines frequently with P Cygni profiles, (b) permitted and forbidden lines of FeII, [FeII], [OI], etc. and (c) strong infrared excess possibly due to thermal radiation from circumstellar dust. They represent one of the two main groups of early-type emission line stars in the Magellanic Clouds (MCs). The other group consists of the classical P Cygni stars and their hotter counterparts, Of-like objects. The S Dor variables, also called Hubble-Sandage variables, are the most extreme variables of the P Cygni and Of-like objects (Stahl et al., 1985). The B[e] supergiants are located in the HR diagram in the same region as S Dor variables and represent evolved evolutionary stages of the most luminous and presumably the most massive O stars (Zickgraf et al., 1986).

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