Semi-major axis a (line), and the heliocentric distance r (dots) versustime t (bottom panel), and the embryo mass M_em versus t (top panel) for the simulation including the gas accretion, with the efficiency factor f_acc = 10⁻⁶. We distinguish the solid (solid) and gaseous (dashed) component of M_em. We used a finer sampling of the orbital elements. Both the migration rates and the eccentricities seem the same as in the nominal case, because the gas accretion contributes only very little to the mass and heating. However, no merging occurred in the course of this simulation. After t ≐ 6400 P_orb, there is an interaction with the disc edge and the evolution is no longer reliable.