Abstract
Nucleosynthesis in type I and type II supernovae is reviewed in the framework of existing models and observational constraints. Major observational constraints for type II supernova (SNII) are the existence of neutron stars in the center of SNII remnants and the observation of hydrogen lines in SNII spectra. The first fact is interpreted by the core bounce mechanism after the onset of a gravitational collapse following core silicon burning of massive stars, leaving a neutron star and ejecting the surrounding envelope. The latter underlines the point that an (evolved) star with an extended hydrogen envelope is the progenitor of such an event. Type I Supernovae (SNI) leave no neutron star remnants and their spectra are characterized by the lack of hydrogen lines. The late time spectra and light curves give evidence for 56Ni-decay. These facts are explained by events where explosive ignition under degenerate conditions takes place (most probably) in accreting white dwarfs, situated in a binary (stellar) system. This mechanism causes the complete disruption of the star. The nucleosynthesis patterns inferred from both models of SNI and SNII are presented and discussed in the light of accompanying uncertainties.
Published Version
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