Volume 405, Number 1, July I 2003
|Page(s)||227 - 229|
|Section||Stellar structure and evolution|
|Published online||16 June 2003|
The circumstellar structure of the Be shell star ϕ Persei
European Southern Observatory, Karl-Schwarzschildstr. 2, 85745 Garching, Germany
2 Astronomical Institute, Academy of Sciences of the Czech Republic, 25165 Ondřejov, Czech Republic
Corresponding author: W. Hummel, email@example.com
We recently modeled the orbital phase variations of the He emission lines of the B2e&sdO shell binary ϕ Per. The angular velocity law used for that study is found to be not correct. We repeated the whole study using a Keplerian velocity law. The application of a Keplerian velocity has only impact on the emission disk radii which are about 50% larger at 15 with respect to our previously used velocity law. All other conclusions remain valid.
Key words: line: formation / line: profiles / stars: circumstellar matter / stars: emission-line, Be / stars: binaries: spectroscopic
© ESO, 2003
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