Can star cluster environment affect dust input from massive AGB stars?
  We examine the fraction of massive asymptotic giant branch (AGB) stars
remaining bound in their parent star clusters and the effect of irradiation of
these stars by intracluster ultraviolet (UV) field. We employ a set of N-body
models of dynamical evolution of star clusters rotating in a galactic potential
at the solar galactocentric radius. The cluster models are combined with
stellar evolution formulae, a library of stellar spectra, and simple models for
SiO photodissociation in circumstellar environment (CSE). The initial stellar
masses of clusters are varied from $50\rm M_\odot$ to $10^{5}\rm M_\odot$.
Results derived for individual clusters are combined using a mass distribution
function for young star clusters. We find that about 30% of massive AGB stars
initially born in clusters become members of the field population, while the
rest evolves in star clusters. They are irradiated by strong intracluster UV
radiation resulting in the decrease of the photodissociation radius of SiO
molecules, in many stars down to the dust formation zone. In absence of dust
shielding, the UV photons penetrate in the CSE deeper than $10R_*$ in 64% and
deeper than $2 R_*$ in 42% of all massive AGB stars. If this suppresses
following dust formation, the current injection rate of silicate dust from AGB
stars in the local Galaxy decreases from $2.2 \times 10^{-4}\rm
M_\odot\,kpc^{-2}\,Gyr^{-1}$ to $1.8 \times 10^{-4}\rm
M_\odot\,kpc^{-2}\,Gyr^{-1}$ at most. A lower revised value of 40% for the
expected fraction of presolar silicate grains from massive AGB stars is still
high to explain the non-detection of these grains in meteorites.
