Pyroclastic Blowout: Dust Survival in Isolated versus Clustered
  Supernovae
  Following the current debate on the fate of SN-condensed dust grains, here we
explore by means of three-dimensional hydrodynamical simulations the
interaction of dusty supernova remnants (SNRs) with the shocked winds of
neighboring massive stars within young massive stellar clusters (SSCs). As a
comparison, we have also explored the evolution of supernova remnants in the
diffuse ISM with constant density. Since the hydrodynamics of SNRs is
intimately related to the properties of their immediate environment, the
lifecycle of dust grains in SNRs within SSCs is radically different from that
in the diffuse ISM. Moreover, off-centered SNRs evolving in the steep density
gradient established due to a star cluster wind experience a blowout phase:
shell fragmentation due to protruding Rayleigh-Taylor instabilities and the
venting of SN ejecta. Our main finding is that clustered SN explosions will
cause a net increase in the amount of dust in the surroundings of young massive
stellar clusters. Our analysis considers the multiple dust processing resulting
from the passage of the SN reverse shock, including its reflection at the SNR's
center, the injection of shocked stellar winds within the respective remnant's
volume and the effect of secondary forward shocks produced in sequential SN
explosions. In the simulations, we have on-the-fly calculated the rates of
thermal sputtering and dust-induced radiative cooling provided an initial
distribution of grain sizes and dust content. Fast-moving elongated dusty SN
ejecta resemble mushroom clouds violently ascending in a stratified atmosphere
after volcanic super-eruptions, where the pyroclasts carried by the clouds are
wind-driven and eventually accumulate into the vast surroundings.
