Super Asymptotic Giant Branch Stars (Super AGBs) lie in the mass range 6-11 Mο, which bridges the divide between low/intermediate mass AGB and massive stars. During the thermally pulsing phase of evolution competition between hot bottom burning (HBB) and third dredge up (3DU) events determine the stellar yields. Obtaining these yields is far more computationally demanding than those of most AGB stars because Super AGBs undergo up to a few thousand thermal pulses. We describe results from evolutionary and nucleosynthetic calculations for these stellar models. We examine element production in these Super AGB stars over time, with results from five metallicities spanning the range Z = 0.02-10−4 ([Fe/H] 0 to −2.3). Super AGB star nucleosynthetic yields have hitherto been neglected in galactic chemical evolution modelling.
|Number of pages||2|
|Publication status||Published - 2012|
|Event||Conference on the Galactic Archaeology - Near-Field Cosmology and the Formation of the Milky Way - |
Duration: 1 Jan 2011 → …
|Conference||Conference on the Galactic Archaeology - Near-Field Cosmology and the Formation of the Milky Way|
|Period||1/01/11 → …|