Volume 383, Number 1, FebruaryIII 2002
|Page(s)||171 - 181|
|Section||Interstellar and circumstellar matter|
|Published online||15 February 2002|
The luminous B[e] binary AS 381
Ritter Observatory, Dept. of Physics & Astronomy, University of Toledo, Toledo, OH 43606-3390, USA
2 Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, Saint-Petersburg 196140, Russia
3 Special Astrophysical Observatory of the Russian Academy of Sciences, Karachai-Cirkassian Republic, Nizhnij Arkhyz 369167, Russia
4 Isaac Newton Institute of Chile, SAO Branch, Russia
5 Ulugh Beg Astronomical Institute of the Uzbek Academy of Sciences, Astronomicheskaya 33, Tashkent 700052, Uzbekistan
6 Issac Newton Institute of Chile, Uzbekistan Branch, Uzbekistan
7 Dept. of Physics and Astronomy, Appalachian State University, Boone, NC 28608, USA
8 ISO Data Centre, Astrophysics Division, Space Science Department of ESA, Villafranca del Castillo, Apartado de Correos 50727, 28080 Madrid, Spain
9 INSA S.A., Villafranca del Castillo, Apartado de Correos 50727, 28080 Madrid, Spain
10 The Aerospace Corp. M2/266, PO Box 92957, Los Angeles, CA 90009, USA
11 Center for Astrophysics and Space Sciences, University of California, San Diego, C-0111, La Jolla, CA 92093, USA
Corresponding author: A. S. Miroshnichenko, firstname.lastname@example.org
Accepted: 22 November 2001
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]). 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 ( mag) suggests that it is located at a distance of ≥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 (~) than the cool one (~7). 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.
Key words: stars: emission-line, Be / stars: individual: AS 381 / techniques: spectroscopic / techniques: photometric
© ESO, 2002
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