Post-He-Burning Phases and Final Fate of Super-AGB Stars

Details Post-He-Burning Phases and Final Fate of Super-AGB Stars Post-He-Burning Phases and Final Fate of Super-AGB Stars

Nov 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..378..133p&link_type=abstract

Why Galaxies Care About AGB Stars: Their Importance as Actors and Probes. ASP Conference Series, Vol. 378, proceedings of the co

Astronomy and Astrophysics

Astronomy

8

Scientific paper

Using the stellar evolution code STAREVOL, we have computed two grids of stellar models (with and without overshooting) that enable us to investigate the role of initial composition, mass loss and convective overshooting on the post-He-burning evolution and final fate (neon-oxygen white dwarf or electron-capture supernova) of stars with initial masses between ˜ 6 and 11 M_&sun;. Our results indicate that the supernova channel for these stars exists, but the initial stellar mass range for this channel is quite narrow (˜ 1 M_&sun; at the most).

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