EAS Publications Series
Volume 13, 2004Evolution of Massive Stars, Mass Loss and Winds
|Page(s)||21 - 62|
|Published online||15 November 2004|
M. Heydari-Malayeri, Ph. Stee and J.-P. Zahn (eds)
EAS Publications Series, 13 (2004) 21-62
Effects of stellar winds and rotation on the evolution of massive stars
Geneva Observatory, 1290 Sauverny, Switzerland
We discuss the impact of the inclusion of both mass loss and rotation in massive star models at different metallicities. Rotation much improves the agreement between theory and observation. In particular rotational mixing allows to produce variations of the surface abundances already during the Main-Sequence phase. The changes of the surface abundances are more important when, for a given initial velocity, the initial mass increases, and/or the initial metallicity decreases. Also the observed high number of red supergiants at low metallicity can be accounted for by rotating stellar models, as well as the observed variation of the number ratio of Wolf-Rayet to O-type stars as a function of the metallicity and the variation with the metallicity of the number ratio of type Ibc to type II supernovae. In all these questions non-rotating models give unsatisfactory fits. Rotating models can also give interesting insights on questions as the origin of the Be stars, the mechanisms responsible for the huge mass loss rates undergone by the Luminous Blue Variables, the sources of primary nitrogen at low metallicity, the rotation rate of pulsars and the progenitors of the collapsars.
© EAS, EDP Sciences, 2004
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.