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Pre-Supernova Evolution of Rotating Massive Stars

  • Raphael Hirschi
  • Georges Meynet
  • André Maeder
  • Stéphane Goriely
Part of the Springer Proceedings in Physics book series (SPPHY, volume 99)

Summary

The Geneva evolutionary code has been modified to study the advanced stages (Ne, O, Si burnings) of rotating massive stars. Here we present the results of four 20 M stars at solar metallicity with initial rotational velocities, υ ini, of 0, 100, 200 and 300 km/s in order to show the crucial role of rotation in stellar evolution. As already known, rotation increases mass loss and core masses [4]. A fast rotating 20 M star has the same central evolution as a non-rotating 26 M. Rotation also increases strongly net total metal yields. Furthermore, rotation changes the SN type so that more SNIb are predicted (see [5] and [6]). Finally, SN1987A-like supernovae progenitor colors can be explained in a single rotating star scenario.

Keywords

Massive Star Core Masse Central Evolution Solar Metallicity Blue Supergiant 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer-Verlag Berlin Heidelberg 2005

Authors and Affiliations

  • Raphael Hirschi
    • 1
  • Georges Meynet
    • 1
  • André Maeder
    • 1
  • Stéphane Goriely
    • 2
  1. 1.Observatoire de GenèveSauvernySwitzerland
  2. 2.Université Libre de BruxellesBruxellesBelgique

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