The evolution of very luminous stars. I - Presupernova evolution

Details The evolution of very luminous stars. I - Presupernova evolution The evolution of very luminous stars. I - Presupernova evolution

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...167..265l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 167, Oct. 1986, p. 265-273.

Astronomy and Astrophysics

Astrophysics

47

Main Sequence Stars, Stellar Evolution, Stellar Luminosity, Stellar Models, Supermassive Stars, Wolf-Rayet Stars, Cassiopeia A, Electron-Positron Pairs, Nuclear Fusion, Stellar Winds, Supernova Remnants

Scientific paper

The presupernova evolution up to the end of central helium burning of a 100 solar mass star of Population I initial composition is presented. Data favor only small amounts of overshooting in such massive stars, and the nucleosynthesis yield due to stellar wind is shown to be compatible with the observed abundances in the material of the quasi-stationary flocculi of the supernova remnant Cas A. Following the quasi-static evolution, the star becomes a massive Wolf-Rayet star consisting primarily of oxygen, with traces of carbon, neon, and magnesium, and the ensuing evolution moves towards the region of electron-positron pair creation instability independent of overshooting.

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