the outer edge of a protoplanetary disc due to photo-evaporative winds can be of the order of $10^{-8} - 10^{-7}\, {\mbox{$\mathrm{M}_{\odot}$}}/ \mathrm{yr}$, see their Fig. 12. We do not take radiative processes into account in this work but we note that any mass loss from the disc, additional to that found in this work, will shorten its lifetime with respect to our findings.

Numerical set-up {#sec:set-up_eda1}
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![A schematic overview of the numerical set-up.\[fig:schematics\_eda1\]](Schematics.pdf){width="49.00000%"}

Our simulations are performed using the AMUSE environment [@portegies_zwart13; @pelupessy13][^2]. AMUSE is a Python framework in which one can use and combine a variety of astrophysical codes that have been published and well tested by the community, i.e. ‘community codes’. The simulation is set up in Python and AMUSE takes care of the communication between Python and the code(s) that one wishes to use. This way, it is very easy to use the same set-up with different community codes and compare their outcome.

Currently, two different smoothed particle hydrodynamics (SPH) codes are included in AMUSE, i.e. Fi [@pelupessy04] and Gadget2 [@springel05; @springel01]. These two codes solve the dynamics of a self-gravitating hydrodynamic fluid using a Tree gravity solver [@hernquist89]. In this work, we use Gadget2 for 