Issue |
A&A
Volume 383, Number 1, FebruaryIII 2002
|
|
---|---|---|
Page(s) | 171 - 181 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20011711 | |
Published online | 15 February 2002 |
The luminous B[e] binary AS 381
1
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, anatoly@physics.utoledo.edu
Received:
2
November
2001
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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.