  We study the asymptotic giant branch (AGB) evolution of stars with masses
between $1~M_{\odot} - 8.5~M_{\odot}$. We focus on stars with a solar chemical
composition, which allows us to interpret evolved stars in the Galaxy. We
present a detailed comparison with models of the same chemistry, calculated
with a different evolution code and based on a different set of physical
assumptions. We find that stars of mass $\ge 3.5~M_{\odot}$ experience hot
bottom burning at the base of the envelope. They have AGB lifetimes shorter
than $\sim 3\times 10^5$ yr and eject into their surroundings gas contaminated
by proton-capture nucleosynthesis, at an extent sensitive to the treatment of
convection. Low mass stars with $1.5~M_{\odot} \le M \le 3~M_{\odot}$ become
carbon stars. During the final phases the C/O ratio grows to $\sim 3$. We find
a remarkable agreement between the two codes for the low-mass models and
conclude that predictions for the physical and chemical properties of these
stars, and the AGB lifetime, are not that sensitive to the modelling of the AGB
phase. The dust produced is also dependent on the mass: low-mass stars produce
mainly solid carbon and silicon carbide dust, whereas higher mass stars produce
silicates and alumina dust. Possible future observations potentially able to
add more robustness to the present results are also discussed.
