  Context: Stars evolving through the asymptotic giant branch (AGB) phase
provide significant feedback to their host system, in form of both gas enriched
in nuclear-burning products and dust formed in their winds, which they eject
into the interstellar medium. Therefore AGB stars are an essential ingredient
for the chemical evolution of the Milky Way and other galaxies. Aims: We study
AGB models with super-solar metallicity, to complete our large database, so far
extending from metal-poor to solar chemical compositions. We provide chemical
yields for masses in the range 1-8 Msun and metallicities Z=0.03 and Z=0.04. We
also study dust production in this metallicity domain. Methods: We calculated
the evolutionary sequences from the pre main sequence through the whole AGB
phase. We follow the variation of the surface chemical composition to calculate
the chemical yields of the various species and model dust formation in the
winds to determine the dust production rate and the total dust mass produced by
each star during the AGB phase. Results: The physical and chemical evolution of
the star is sensitive to the initial mass: M> 3Msun stars experience hot bottom
burning, whereas the surface chemistry of the lower mass counterparts is
altered only by third dredge-up. The carbon-star phase is reached by
2.5-3.5Msun stars of metallicity Z=0.03, whereas all the Z=0.04 stars (except
the 2.5 Msun) remain O-rich for the whole AGB phase. Most of the dust produced
by metal-rich AGBs is in the form of silicates particles. The total mass of
dust produced increases with the mass of the star, reaching
  ~ 0.012 Msun for 8Msun stars.
