Presupernova evolution of the most massive stars

Details Presupernova evolution of the most massive stars Presupernova evolution of the most massive stars

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ssrv...66..365l&link_type=abstract

Space Science Reviews, Volume 66, Issue 1-4, pp. 365-372

Physics

5

Stellar Evolution, Massive Stars, Mass Loss, Supernovae

Scientific paper

Taking as example a 60M &sun; star of solar metallicity, the state of the art of model calculations for very massive, from the main sequence to the supernova stage, is reviewed. It is argued that — due to the simple internal structure of Wolf-Rayet stars — the post main sequence evolutionary phases are currently those which are better understood. A brief discussion of the supernova outcome from very massive stars is given. Then, the more uncertain main sequence evolution is discussed. A first attempt to incorporate results about pulsational instabilities of very massive stars in stellar evolutionary calculations is performed. On its basis, a new type of evolutionary sequence for very massive stars is obtained, namely O-star → Of-star → H-rich WNL → LBV → H-poor WNL → WNE → WC → SN. This scenario is shown to correspond better to many observed properties of very massive stars than the standard one. It includes a model for the prototype LBV P Cygni.

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