Disc truncation in embedded star clusters: Dynamical encounters versus
  face-on accretion
  Observations indicate that the dispersal of protoplanetary discs in star
clusters occurs on time scales of about 5 Myr. Several processes are thought to
be responsible for this disc dispersal. Here we compare two of these processes:
dynamical encounters and interaction with the interstellar medium, which
includes face-on accretion and ram pressure stripping. We perform simulations
of embedded star clusters with parameterisations for both processes to
determine the environment in which either of these processes is dominant. We
find that face-on accretion, including ram pressure stripping, is the dominant
disc truncation process if the fraction of the total cluster mass in stars is
$\lesssim 30\,\%$ regardless of the cluster mass and radius. Dynamical
encounters require stellar densities $\gtrsim 10^4$ pc$^{-3}$ combined with a
mass fraction in stars of $\approx 90\,\%$ to become the dominant process. Our
results show that during the embedded phase of the cluster, the truncation of
the discs is dominated by face-on accretion and dynamical encounters become
dominant when the intra-cluster gas has been expelled. As a result of face-on
accretion the protoplanetary discs become compact and their surface density
increases. In contrast, dynamical encounters lead to discs that are less
massive and remain larger.
