Growth tracks of planets that accrete pebbles in an evolving protoplanetary disc. The planets are placed in discs with different water-to-silicate ratios at a disc evolution time of t₀ = 2 Myr. The simulations are stopped when t_f = 3 Myr is reached, meaning the planet and disc evolve for 1 Myr. Note that the different resulting planetary masses and orbital distances are a result of the different underlying disc structures (Fig. 2) and migration patters (Fig. 3).