Pre-Supernova Evolution of Rotating Massive Stars
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 . 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  and ). Finally, SN1987A-like supernovae progenitor colors can be explained in a single rotating star scenario.
KeywordsMassive Star Core Masse Central Evolution Solar Metallicity Blue Supergiant
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- 2.R. Hirschi et al.: astro-ph 0301357 (2003)Google Scholar