The circumstellar structure of the Be shell star phi Persei. II. Modeling

Details The circumstellar structure of the Be shell star phi Persei. II. Modeling The circumstellar structure of the Be shell star phi Persei. II. Modeling

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...405..227h&link_type=abstract

Astronomy and Astrophysics, v.405, p.227-229 (2003)

Astronomy and Astrophysics

Astrophysics

Line: Formation, Line: Profiles, Stars: Circumstellar Matter, Stars: Emission-Line, Be, Stars: Binaries: Spectroscopic

Scientific paper

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.

Affiliated with

Also associated with

No associations

Rating

The circumstellar structure of the Be shell star phi Persei. II. Modeling does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The circumstellar structure of the Be shell star phi Persei. II. Modeling, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The circumstellar structure of the Be shell star phi Persei. II. Modeling will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1461812