Hostname: page-component-745bb68f8f-b95js Total loading time: 0 Render date: 2025-01-13T05:24:56.695Z Has data issue: false hasContentIssue false
  • English
  • Français

The influence of mass loss by stellar wind on the evolution of massive helium burning stars

Published online by Cambridge University Press:  12 April 2016

D. Vanbeveren
D. Vanbeveren*
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel, Belgium

Extract

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.

Helium burning stars with masses between 10 Mo and 40 Mo are evolved up to core helium exhaustion including mass loss by stellar wind at rates between 10-5 Mo/yr and 10-4 Mo/yr appropriate for WR stars. Different M formalisms were used. It should however be noted that the results presented here are only marginally dependent on this formalism. The initial models contain a small hydrogen shell. The atmospherical hydrogen abundance Xatm = 0.2-0.3. These models correspond to primary remnants (with hydrogen ZAMS masses between 30 M0 and 100 M0) after a case B mode of mass transfer in close binaries, or to stars after a red giant phase of huge mass loss comparable to late case B remnants after Roche lobe overflow. Evolutionary details can be found elsewhere (Vanbeveren, D., Ph.D. Thesis, Vrije Universiteit Brussel) and will not be discussed here. I want to focus on two applications

Type
Session V - Mass Loss and Stellar Evolution: Massive Stars
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 275 - 278
Copyright
Copyright © Reidel 1981