almost 40% of the discs is smaller than 100 AU and the median disc radius can be as small as 20 AU in the core. Close stellar encounters thus affect the surface area of the disc and thereby also the rate at which the disc can sweep up ISM. In this work we only focus on the hydrodynamic aspects of accretion onto protoplanetary discs, in particular the accretion rate. The disc radius we find in our simulations is of similar size as the 20 AU found by @vincke15. The question whether the process of ram pressure or dynamical encounters dominates the truncation of the disc in embedded dense stellar systems is beyond the scope of this paper.

External photo-evaporation
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Globular clusters host a large number of massive stars in the early phases of their evolution and the large UV flux they produce may also strip material from the disc. Studies have shown that the fraction of stars that have discs can decrease by a factor of two close to O stars [see e.g. @balog07; @guarcello07; @guarcello09; @fang12], but @richert15 argue that these results could be partly affected by sample incompleteness. Recently, @facchini16 estimated that the mass loss rate from 