Cartoon of the code construction used to simulate the planet formation process from dust grains to full-sized planets. The evolution of dust and pebbles and planetesimal formation are treated by the Lagrangian code (“L-code”), which covers the entire disk. Planetesimals form just outside the snowline, and their growth and migration are followed with an N-body code (“N-code”), which accounts for dynamics, planetesimal and pebble accretion, gas drag, and type-I migration. When protoplanets migrate across the inner domain radius of the N-code r_domain, their final growth stage is calculated with a semi-analytic model (“A-code”). The way in which the codes are coupled in time is discussed in Sect. 2.4.