We present a new grid of stellar models and nucleosynthetic yields for super-AGB stars with metallicities Z=0.001 and 0.0001 , applicable for use within galactic chemical evolution models .
Contrary to more metal rich stars where hot bottom burning is the main driver of the surface composition , in these lower metallicity models the effect of third dredge-up and corrosive second dredge-up also have a strong impact on the yields .
These metal-poor and very metal-poor super-AGB stars create large amounts of ^ { 4 } He , ^ { 13 } C and ^ { 14 } N , as well as the heavy magnesium isotopes ^ { 25 } Mg and ^ { 26 } Mg .
There is a transition in yield trends at metallicity Z \approx 0.001 , below which we find positive yields of ^ { 12 } C , ^ { 16 } O , ^ { 15 } N , ^ { 27 } Al and ^ { 28 } Si , which is not the case for higher metallicities .
We explore the large uncertainties derived from wind prescriptions in super-AGB stars , finding \approx 2 orders of magnitude difference in yields of ^ { 22 } Ne , ^ { 23 } Na , ^ { 24 , 25 , 26 } Mg , ^ { 27 } Al and our s-process proxy isotope g .
We find inclusion of variable composition low temperature molecular opacities is only critical for super-AGB stars of metallicities below Z \approx 0.001 .
We analyze our results , and those in the literature , to address the question : Are super-AGB stars the polluters responsible for extreme population in the globular cluster NGC 2808 ?
Our results , as well as those from previous studies , seem unable to satisfactorily match the extreme population in this globular cluster .