our reference model and we verify the consistency and robustness of our results by comparing with Fi. Both SPH codes include self-gravity.

Because we want to be able to perform future simulations for a wide range of parameters, we need to find a balance between computational effort and convergence, i.e. the most efficient set-up. In order to test whether our particle resolution is sufficient, we perform simulations with different numbers of particles in the disc. This way, we can test whether the results converge and the numerical noise diminishes. The verification and validation will be discussed in Sec. \[sec:convergence\_eda1\].

For our reference model, we use the vanilla version of Gadget2 as it is freely available online[^3] and included in AMUSE, with the only exception that we have implemented the @morris97 viscosity formalism as is done in M09, see Sec. \[sec:visc\_eda1\].

The set-up of our simulations is as follows (see Fig. \[fig:schematics\_eda1\]): a stationary protoplanetary disc is positioned coaxially in a cylindrical, laminar flow of gas, representing the ISM. The protoplanetary disc is positioned in the centre of the cylinder. The inflow and outflow boundaries are each located at a distance of 500 AU from the centre of the protoplanetary disc. 