Formation and early evolution of 10 M_♃ planets forming at 5.2 AU. The thin red line is for hot accretion (HS). The remaining four cases are all for cold accretion, but differ in the initial planetesimal surface density Σ_s,0 as indicated in the plot. The top left panel shows the core (solid) and total mass (dotted lines). The top right panel shows the total luminosity. The bottom left and right panels are the specific entropy at the core-envelope boundary, and the outer radius, respectively. Note how the luminosity, entropy and radius at the end of the formation phase increase with core mass for cold accretion.