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We have computed detailed evolution and nucleosynthesis models for super andmassive AGB stars over the mass range 6.5-9.0 Msun in divisions of 0.5 Msunwith metallicities Z=0.02, 0.008 and 0.004. These calculations, in which wefind third dredge-up and hot bottom burning, fill the gap between existing lowand intermediate-mass AGB star models and high mass star models that becomesupernovae. For the considered metallicities, the composition of the yields islargely dominated by the thermodynamic conditions at the base of the convectiveenvelope rather than by the pollution arising from third dredge up. Weinvestigate the effects of various uncertainties, related to the mass-lossrate, mixing length parameter, and the treatment of evolution after theenvelope instability that develops near the end of the (Super)AGB phase.Varying these parameters alter the yields mainly because of their impact on theamount of third dredge up enrichment, and to a lesser extent on the hot bottomburning conditions. Our models produce significant amounts of He4, Li7(depending on the mass-loss formulation) C13, N14, O17, Na23, Mg25, as well theradioactive isotope Al26 in agreement with previous investigation. In additionour results show enrichment of Ne22, Mg26 and Fe60, as well as a substantialincrease in our proxy neutron capture species representing all species heavierthan iron. These stars may provide important contributions to the Galaxy'sinventory of the heavier Mg isotopes, N14, Li7 and Al27.

Super and Massive AGB Stars: II - Nucleosynthesis and Yields - Z=0.02, 0.008 and 0.004