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We examine the fraction of massive asymptotic giant branch (AGB) starsremaining bound in their parent star clusters and the effect of irradiation ofthese stars by intracluster ultraviolet (UV) field. We employ a set of N-bodymodels of dynamical evolution of star clusters rotating in a galactic potentialat the solar galactocentric radius. The cluster models are combined withstellar evolution formulae, a library of stellar spectra, and simple models forSiO photodissociation in circumstellar environment (CSE). The initial stellarmasses 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 distributionfunction for young star clusters. We find that about 30% of massive AGB starsinitially born in clusters become members of the field population, while therest evolves in star clusters. They are irradiated by strong intracluster UVradiation resulting in the decrease of the photodissociation radius of SiOmolecules, in many stars down to the dust formation zone. In absence of dustshielding, the UV photons penetrate in the CSE deeper than $10R_*$ in 64% anddeeper than $2 R_*$ in 42% of all massive AGB stars. If this suppressesfollowing dust formation, the current injection rate of silicate dust from AGBstars in the local Galaxy decreases from $2.2 \times 10^{-4}\rmM_\odot\,kpc^{-2}\,Gyr^{-1}$ to $1.8 \times 10^{-4}\rmM_\odot\,kpc^{-2}\,Gyr^{-1}$ at most. A lower revised value of 40% for theexpected fraction of presolar silicate grains from massive AGB stars is stillhigh to explain the non-detection of these grains in meteorites.

Can star cluster environment affect dust input from massive AGB stars?