  We extend the formalism presented in our recent calculations of dust ejecta
from the Thermally Pulsing Asymptotic Giant Branch (TP-AGB) phase, to the case
of super-solar metallicity stars. The TP-AGB evolutionary models are computed
with the COLIBRI code. We adopt our preferred scheme for dust growth. For
M-giants, we neglect chemisputtering by H$_2$ molecules and, for C-stars we
assume a homogeneous growth scheme which is primarily controlled by the carbon
over oxygen excess. At super-solar metallicities, dust forms more efficiently
and silicates tend to condense significantly closer to the photosphere (r~1.5
R$_*$) - and thus at higher temperatures and densities - than at solar and
sub-solar metallicities (r~2-3 R$_*$). In such conditions, the hypothesis of
thermal decoupling between gas and dust becomes questionable, while dust
heating due to collisions plays an important role. The heating mechanism delays
dust condensation to slightly outer regions in the circumstellar envelope. We
find that the same mechanism is not significant at solar and sub-solar
metallicities. The main dust products at super-solar metallicities are
silicates. We calculate the total dust ejecta and dust-to-gas ejecta, for
various values of the stellar initial masses and initial metallicities Z=0.04,
0.06. Merging these new calculations with those for lower metallicities it
turns out that, contrary to what often assumed, the total dust-to-gas ejecta of
intermediate-mass stars exhibit only a weak dependence on the initial metal
content.
