In situ formation of a 1 M_⊕ planet at 6 AU for different radii of accreted planetesimals (red, 100 km; blue, 10 km; green, 1 km; orange, 0.1 km). The solid line is for the equilibrium approximation of eccentricities and inclinations (see Eqs. (56), (57)). The dashed and dotted lines are for the explicit calculation of e and i solving the differential equations Eqs. (31), (32). Two different initial values, e₀, i₀, were considered: the dashed line represents the case where e₀ and i₀ are given by Eqs. (59), (58), while the dotted line assumes e₀, i₀ to be the initial equilibrium values of the equilibrium case. The top-left panel depicts the mass growth of the protoplanet as a function of time. The top-right panel shows the time evolution of the eccentricity. The bottom-left panel shows the eccentricity as a function of the mass of the embryo. Clearly, in all cases, equilibrium is attained after an out of equilibrium state. The bottom-right panel plots the accretion rate of solids as a function of the embryo mass. Note that, as a function of the planet mass, the difference in the accretion rate is only a consequence of the difference in e and i.