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 \geq 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 } \leq M \leq 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 .