The luminous B[e] binary AS 381

Details The luminous B[e] binary AS 381 The luminous B[e] binary AS 381

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002a%26a...383..171m&link_type=abstract

Astronomy and Astrophysics, v.383, p.171-181 (2002)

Astronomy and Astrophysics

Astrophysics

8

Stars: Emission-Line, Be, Stars: Individual: As 381, Techniques: Spectroscopic, Techniques: Photometric

Scientific paper

We present the results of optical and near-IR spectroscopic and broadband multicolour photometric observations of the emission-line star AS 381. Its properties were found to be similar to those of Be stars with warm dust, a group of galactic objects recently defined by Sheikina et al. (\cite{smc}). The spectrum of AS 381 indicates the presence of both a hot (early B-type) and a cool (K-type) star in the system. A high interstellar reddening (AV ~ 7 mag) suggests that it is located at a distance of ge 3 kpc, and the companions have luminosity types II or higher. The emission-line profiles indicate that the system is surrounded by a flattened circumstellar envelope, which is viewed close to pole-on. The hot companion is found to be ~ 2 mag brighter in the V-band and more massive ( ~ 20 Msun) than the cool one ( ~ 7 Msun). The strong line emission and position of the companions in the Hertzsprung-Russell diagram indicate that the system is experiencing mass exchange. We suggest that AS 381 is the first B[e] supergiant binary discovered in the Milky Way.

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