Maximum central temperature T_c,max for 10 km ≤ R ≤ 200 km, t₀ = 0 Myr and t_ac varying according to the accretion scenarios from Table 4. Upper left panel: asteroid belt, dust/ice = 3∕1. Middle left panel: inter-planet disk, dust/ice = 3∕1. Upper right panel: Kuiper belt, dust/ice = 3∕1. Middle right panel: Kuiper belt, dust/ice = 1∕1. Lower panel:final structures of initially icy planetesimals, numbered 1 through 6 according to the degree of differentiation. Not all of the structures are obtained for the accretion at different heliocentric distances (see Table 5 for an overview). Hydration of silicates is indicated by the dashed blue lines, starting at the water ice melting temperature of 273 K (serpentinization at 273 K takes ≈200 days according to Wakita & Sekiya (2011) and Jones & Brearley (2006); the temperature interval of 320− 520 K has been suggested by Allen & Seyfried 2004). We note that consideration of endothermic processes, such as melting of metal and silicates, could reduce the temperature and shift the isolines with T > 1260 K slightly to earlier accretion times and larger radii.