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This article is an erratum for: [this article]

Issue A&A
Volume 405, Number 1, July I 2003
Page(s) 227 - 229
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20030572



A&A 405, 227-229 (2003)
DOI: 10.1051/0004-6361:20030572

Erratum

The circumstellar structure of the Be shell star $\phi$ Persei

II. Modeling
W. Hummel1 and S. Stefl2

1  European Southern Observatory, Karl-Schwarzschildstr. 2, 85745 Garching, Germany
2  Astronomical Institute, Academy of Sciences of the Czech Republic, 25165 Ondrejov, Czech Republic

Erratum of A&A  368 p. 471


Abstract
(A&A, 368, 471-483 (2001), DOI: 10.1051/0004-6361:20000559)

We recently modeled the orbital phase variations of the He emission lines of the B2e&sdO shell binary $\phi$ 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 R* 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

Offprint request: W. Hummel, whummel@eso.org




© ESO 2003


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