Possible scenario of the dynamical history of the four giant planets of our Solar System if they were to form in a cold low-viscosity protoplanetary disc and then interact with a 50 M_⊕ planetesimal disc located at 0.5 au away from the last planet. In this scenario the initial planetary system is composed of five planets, where the fifth planet is a 6 M_⊕ planet that could correspond to P9. The first 800 kyr show a hydrodynamical simulation of the protoplanetary disc phase, in which the planets migrate into a resonant configuration. In the background we show the radial profiles of the gas surface density in the disc. We then simulate a mock gas-dispersal period (between the two white dashed lines). Finally, we show the result of one N-body simulation in which the planets interact with a planetesimal disc. The system goes unstable quickly and ejects the fifth planet before 2 Myr. We then integrate the system for a few billion years (with a change in scaling of the x-axis from linear to logarithmic) and obtain a good analogue of the present Solar System (the triangles mark the actual semi-major axes of the giant planets).