Equatorial mass loss from Be stars
Abstract
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.
Keywords
Cite
@article{arxiv.1010.1019,
title = {Equatorial mass loss from Be stars},
author = {Cyril Georgy and Sylvia Ekström and Anahí Granada and Georges Meynet},
journal= {arXiv preprint arXiv:1010.1019},
year = {2015}
}
Comments
2 pages, 2 figures To appear in the proceedings of the IAUS 272 on "Active OB stars: structure, evolution, mass loss and critical limits"