| Issue |
A&A
Volume 480, Number 1, March II 2008
|
|
|---|---|---|
| Page(s) | 213 - 214 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20079024 | |
| Published online | 09 January 2008 | |
Research Note
No Be binary component in the eclipsing binary DW Carinae
Astronomical Institute of the Charles University, Faculty of Mathematics and Physics, V Holešovičkách 2, 180 00 Praha 8, Czech Republic e-mail: hec@sirrah.troja.mff.cuni.cz
Received:
8
November
2007
Accepted:
22
December
2007
In a recent excellent study by Southworth and Clausen, refined orbital elements and basic physical properties of DW Carinae were derived. A suggestion was made that this binary is a Be-star system since a double, Hα emission line was observed. I argue that the observed Hα emission is nebular emission from the Carina nebula and that neither of the binary components of DW Carinae is a Be star.
Key words: binaries: eclipsing / stars: early-type / stars: fundamental parameters / stars: emission-line, Be / stars: individual: DW Carinae
© ESO, 2008
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