The circumstellar structure of the be shell star φ Persei -: II.: Modeling (vol 368, pg 471, 2001)

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.