  We calculate the dust formed around AGB and SAGB stars of metallicity Z=0.008
by following the evolution of models with masses in the range 1M<M<8M
throughthe thermal pulses phase, and assuming that dust forms via condensation
of molecules within a wind expanding isotropically from the stellar surface. We
find that, because of the strong Hot Bottom Burning (HBB) experienced, high
mass models produce silicates, whereas lower mass objects are predicted to be
surrounded by carbonaceous grains; the transition between the two regimes
occurs at a threshold mass of 3.5M. These fndings are consistent with the
results presented in a previous investigation, for Z=0.001. However, in the
present higher metallicity case, the production of silicates in the more
massive stars continues for the whole AGB phase, because the HBB experienced is
softer at Z=0.008 than at Z=0.001, thus the oxygen in the envelope, essential
for the formation of water molecules, is never consumed completely. The total
amount of dust formed for a given mass experiencing HBB increases with
metallicity, because of the higher abundance of silicon, and the softer HBB,
both factors favouring a higher rate of silicates production. This behaviour is
not found in low mass stars,because the carbon enrichment of the stellar
surface layers, due to repeated Third Drege Up episodes, is almost independent
of the metallicity. Regarding cosmic dust enrichment by intermediate mass
stars, we find that the cosmic yield at Z=0.008 is a factor 5 larger than at
Z=0.001. In the lower metallicity case carbon dust dominates after about 300
Myr, but at Z=0.008 the dust mass is dominated by silicates at all times,with a
prompt enrichment occurring after about 40 Myr, associated with the evolution
of stars with masses M =7.5 -8M.
