  Both simulations and observations indicate that stars form in filamentary,
hierarchically clustered associations, most of which disperse into their
galactic field once feedback destroys their parent clouds. However, during
their early evolution in these substructured environments, stars can undergo
close encounters with one another that might have significant impacts on their
protoplanetary disks or young planetary systems. We perform N-body simulations
of the early evolution of dissolving, substructured clusters with a wide range
of properties, with the aim of quantifying the expected number and orbital
element distributions of encounters as a function of cluster properties. We
show that the presence of substructure both boosts the encounter rate and
modifies the distribution of encounter velocities compared to what would be
expected for a dynamically relaxed cluster. However, the boost only lasts for a
dynamical time, and as a result the overall number of encounters expected
remains low enough that gravitational stripping is unlikely to be a significant
effect for the vast majority of star-forming environments in the Galaxy. We
briefly discuss the implications of this result for models of the origin of the
Solar System, and of free-floating planets. We also provide tabulated encounter
rates and orbital element distributions suitable for inclusion in population
synthesis models of planet formation in a clustered environment.
