HR diagrams of the H-burning post-AGB sequences we computed for different masses and initial metallicities. Tracks are presented from the beginning of the post-AGB phase when the H-rich envelope drops below M_env = 0.01 M_⋆ to the moment in which the star has already entered its white dwarf cooling sequence at L_⋆ = L_⊙. At that point gravitational settling should have already started to turn post-AGB stars into DA-WDs, a process not included in the present computations. Red lines indicate computed isochrones for different ages since the zero point defined at log T_eff = 3.85. Thin gray lines in the Z₀ = 0.001 and Z₀ = 0.0001 panels correspond to the evolution of the M_i = 0.8 M_⊙ He-burning sequences shown in Fig. 10 (M_f = 0.4971 M_⊙ and 0.5183 M_⊙, respectively).