Stellar yields from metal-rich asymptotic giant branch models
  We present new theoretical stellar yields and surface abundances for three
grids of metal-rich asymptotic giant branch (AGB) models. Post-processing
nucleosynthesis results are presented for stellar models with initial masses
between 1$M_{\odot}$ and 7.5$M_{\odot}$ for $Z=0.007$, and 1$M_{\odot}$ and
8$M_{\odot}$ for $Z=0.014$ (solar) and $Z=0.03$. We include stellar surface
abundances as a function of thermal pulse on the AGB for elements from C to Bi
and for a selection of isotopic ratios for elements up to Fe and Ni (e.g.,
$^{12}$C/$^{13}$C), which can be obtained from observations of molecules in
stars and from the laboratory analysis of meteoritic stardust grains. Ratios of
elemental abundances of He/H, C/O, and N/O are also included, which are useful
for direct comparison to observations of AGB stars and their progeny including
planetary nebulae. The integrated elemental stellar yields are presented for
each model in the grid for hydrogen, helium and all stable elements from C to
Bi. Yields of Li are also included for intermediate-mass models with hot bottom
burning. We present the first $slow$ neutron-capture ($s$-process) yields for
super-solar metallicity AGB stars with $Z=0.03$, and the first complete
$s$-process yields for models more massive than 6$M_{\odot}$ at all three
metallicities.
