Hostname: page-component-7c8c6479df-5xszh Total loading time: 0 Render date: 2024-03-28T21:04:25.685Z Has data issue: false hasContentIssue false

Evolution of the First Stars: the major role of rotation for mixing and mass loss

Published online by Cambridge University Press:  23 December 2005

André Maeder
Affiliation:
Geneva Observatory, CH–1290 Sauverny, Switzerland, email: andre.maeder@obs.unige.ch, email: georges.meynet@obs.unige.ch, email: sylvia.ekstrom@obs.unige.ch
Georges Meynet
Affiliation:
Geneva Observatory, CH–1290 Sauverny, Switzerland, email: andre.maeder@obs.unige.ch, email: georges.meynet@obs.unige.ch, email: sylvia.ekstrom@obs.unige.ch
Sylvia Ekström
Affiliation:
Geneva Observatory, CH–1290 Sauverny, Switzerland, email: andre.maeder@obs.unige.ch, email: georges.meynet@obs.unige.ch, email: sylvia.ekstrom@obs.unige.ch
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We show that rotation plays a major role for very low metallicity stars, even if the distribution of angular velocities $\Omega$ with respect to critical values is the same as at solar $Z$. The internal gradients of $\Omega$ are much larger at lower metallicity $Z$, which enhance internal mixing and give rise to N-enrichments. Low $Z$ stars easily reach break–up during MS evolution and lose mass. They also lose mass as red giants or supergiants due to their surface enrichments in heavy elements. The winds of low $Z$ stars make peculiar contributions to the chemical yields. We suggest that the helium rich blue Main Sequence (bMS) of $\omega$ Centauri bears the signature of such enrichments by the stellar winds of rotating stars in the first stellar generations.

Type
Contributed Papers
Copyright
© 2005 International Astronomical Union