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Pre-Supernova Evolution of Rotating Massive Stars

Published online by Cambridge University Press:  19 September 2016

Raphael Hirschi ,
Georges Meynet ,
André Maeder  and
Stéphane Goriely
Raphael Hirschi
Affiliation:
Observatoire de Genève, 1290 Sauverny, Switzerland;[email protected]
Georges Meynet
Affiliation:
Observatoire de Genève, 1290 Sauverny, Switzerland;[email protected]
André Maeder
Affiliation:
Observatoire de Genève, 1290 Sauverny, Switzerland;[email protected]
Stéphane Goriely
Affiliation:
Université Libre de Bruxelles, Bruxelles, Belgique

Summary

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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, vini, 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.

Type
Part III Supernovae: Progenitors/Remnants
Information
International Astronomical Union Colloquium , Volume 192: Cosmic Explosions , 2005 , pp. 209 - 213
Copyright
Copyright © Springer-Verlag 2005

References

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