The post-He-burning evolution and final fate of Super-AGB stars, and the associated nucleosynthesis

Details The post-He-burning evolution and final fate of Super-AGB stars, and the associated nucleosynthesis The post-He-burning evolution and final fate of Super-AGB stars, and the associated nucleosynthesis

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006phdt........37p&link_type=abstract

PhD Thesis, Catania University, 2006

Astronomy and Astrophysics

Astrophysics

8

Stars: Evolution, Stars: Interiors, Stars: Agb, Nucleosynthesis, Abundances

Scientific paper

The so-called Super-AGB stars have initial mass between M_{up} (minimum initial mass above which C-burning ignites) and M_{mas} (minimum initial mass for the completion of all the nuclear burning phases leading to an iron-core collapse supernova). Thus these stars are massive enough to ignite carbon but, being unable to evolve through all nuclear burning stages, they end their life either forming a neon-oxygen white dwarf (NeO WD) or going through an electron-capture supernova becoming a neutron star (NS), if electron-capture reactions are efficiently activated. The fraction of Super-AGB stars evolving into each of these channels and their post-He-burning evolution as well as their correlated nucleosynthesis have not yet been explicitly investigated. We address these issues based on two grids (with and without overshooting) of stellar models, investigating the effects of initial mass, initial composition, mass loss and convective overshooting. Moreover we pay attention to the ``boundaries'' (M_{up} and M_{mas}) of the Super-AGB stars as well as to the critical mass M_N, setting the transition between Super-AGB stars that evolve into a NeO WD and the ones that become NSs. The impact of the results in relation to different astrophysical issues is also discussed.

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