| Issue |
A&A
Volume 405, Number 1, July I 2003
|
|
|---|---|---|
| Page(s) | 227 - 229 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20030572 | |
| Published online | 16 June 2003 | |
The circumstellar structure of the Be shell star ϕ Persei
II. Modeling
1
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, whummel@eso.org
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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