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We discuss the dust chemistry and growth in the circumstellar envelopes(CSEs) of Thermally Pulsing Asymptotic Giant Branch (TP-AGB) star modelscomputed with the COLIBRI code, at varying initial mass and metallicity(Z=0.001, 0.008, 0.02, 0.04, 0.06). A relevant result of our analysis dealswith the silicate production in M-stars. We show that, in order to reproducethe observed trend between terminal velocities and mass-loss rates in GalacticM-giants, one has to significantly reduce the efficiency of chemisputtering byH2 molecules, usually considered as the most effective dust destructionmechanism. This indication is also in agreement with the most recent laboratoryresults, which show that silicates may condense already at T=1400 K, insteadthan at Tcond=1000 K, as obtained by models that include chemisputtering. Fromthe analysis of the total dust ejecta, we find that the total dust-to-gasejecta of intermediate-mass stars are much less dependent on metallicity thanusually assumed. In a broader context, our results are suitable to study thedust enrichment of the interstellar medium provided by TP-AGB stars in bothnearby and high redshift galaxies.

Dust production from sub-solar to super-solar metallicity in Thermally Pulsing Asymptotic Giant Branch Stars