  Low and intermediate mass stars with super solar metallicities comprise a
known portion of the universe. Yet yields for asymptotic giant branch (AGB)
stars with metallicities greater than $Z=0.04$ do not exist in the literature.
This contributes a significant uncertainty to galactic chemical evolution
simulations. We present stellar yields of AGB stars for $M=1-8$$M_\odot$ and
$Z=0.04-0.10$. We also weight these yields to represent the chemical
contribution of a metal-rich stellar population. We find that as metallicity
increases, the efficiency of the mixing episodes (known as the third dredge up)
on the thermally pulsing AGB (TP-AGB) decrease significantly. Consequently,
much of the nucleosynthesis that occurs on the TP-AGB is not represented on the
surface of very metal-rich stars. It instead remains locked inside the white
dwarf remnant. The temperatures at the base of the convective envelope also
decrease with increasing metallicity. For the intermediate mass models, this
results in the occurrence of only partial hydrogen burning at this location, if
any burning at all. We also investigate heavy element production via the slow
neutron capture process (s-process) for three 6$M_\odot$ models: $Z=0.04, 0.05$
and $0.06$. There is minor production at the first s-process peak at strontium,
which decreases sharply with increasing metallicity. We find the chemical
contributions of our models are dominated by proton capture nucleosynthesis,
mixed to the surface during first and second dredge up events. This conclusion
is mirrored in our stellar population yields, weighted towards the lower mass
regime to reflect the mass distribution within a respective galaxy.
