Equatorial mass loss from Be stars

Details Equatorial mass loss from Be stars Equatorial mass loss from Be stars

2010-10-05

arxiv.org/abs/1010.1019v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

2 pages, 2 figures To appear in the proceedings of the IAUS 272 on "Active OB stars: structure, evolution, mass loss and criti

Scientific paper

Be stars are thought to be fast rotating stars surrounded by an equatorial disc. The formation, structure and evolution of the disc are still not well understood. In the frame of single star models, it is expected that the surface of an initially fast rotating star can reach its keplerian velocity (critical velocity). The Geneva stellar evolution code has been recently improved, in order to obtain some estimates of the total mass loss and of the mechanical mass loss rates in the equatorial disc during the whole critical rotation phase. We present here the first results of the computation of a grid of fast rotating B stars evolving towards the Be phase, and discuss the first estimates we obtained.

Affiliated with

Also associated with

No associations

Rating

Equatorial mass loss from Be stars 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 Equatorial mass loss from Be stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Equatorial mass loss from Be stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-426900