Evolution of a single planet in a disc with a DZ (left) and at the IB (right). Top: migration path, a(t). In each panel, every line belongs to a separate simulation with only one planet. Bottom: surface density profiles at t = 50 (black), when the full potential of the planet is applied on the disc, and t = 10⁴ orbit. The colour code is the same as for the top row and the final locations of the planets are marked by circles. The low-mass planet is trapped the DZ model and slowly migrates outwards in the IB model. In contrast, the massive planet (Jupiter mass) continues its migration to the inner disc because of the deformation of the bump by its gap.