Hostname: page-component-77c89778f8-fv566 Total loading time: 0 Render date: 2024-07-20T14:14:44.790Z Has data issue: false hasContentIssue false
  • English
  • Français

Instabilities in Very Massive Stars

Published online by Cambridge University Press:  12 April 2016

Knut Jørgen  and
Røed Ødegaard
Knut Jørgen
Affiliation:
Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, N-0315 Oslo, Norway
Røed Ødegaard
Affiliation:
Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, N-0315 Oslo, Norway

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.

Detailed dynamical models and nucleosynthesis yields of very massive stars from early pre-MS through very late stages have been computed. The recent reduction of mass loss rates for the WR stages can have important consequences for both the evolution, surface composition and stability. Depending on mass and metallicity, in the present models instabilities occur during the accretion phase (pre-ZAMS), LBV stage and very late stages (WC).

Type
Part 5. Theoretical Models of Classical Pulsating Stars
Information
International Astronomical Union Colloquium , Volume 176: The Impact of Large-Scale Surveys on Pulsating Star Research , 2000 , pp. 391 - 392
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Ødegaard, K.J.R. 1999, in Lecture Notes in Physics, Vol. 523, Variable and Non-Spherical Stellar Winds in Luminous Hot Stars, ed. Wolf, B., Stahl, O. & Fullerton, A.W. (Berlin: Springer), 353 Google Scholar