Core growth as function of time, plotted for various orbital distances (0.5,5 and 50 AU). The drift branch, marked by grey solid lines, assumes an initial core mass of M₀ = 10^-5M_⊕ and Δ = 0.05. The drift growth continues until the transition mass M_t is reached (marked by a full grey dot). Accretion continues through the more efficient Hill branch, drawn in black. For clarity, we start the Hill growth from the transition mass at time t = 0 yr, instead of continuing from the time where drift accretion comes to a halt. The masses of Ceres and Pluto (located at respectively 2.7 and 39 AU) are marked on the vertical axis for reference. The grey dotted curves correspond to classical planetesimal accretion (PA), where the faster growth corresponds to 2D accretion of planetesimal fragments (Rafikov 2004) and the slower to 3D accretion of planetesimals (e.g. Dodson-Robinson et al. 2009). Note that drift accretion timescale at 50 AU takes more than 10⁸ yr and its transition mass point is not plotted.