First example of a system in which the secondary initiates the first mass transfer phase while the primary has already evolved to the WD stage. In this case the interplay between LK cycles, stellar evolution and tides shrinks the inner orbit in consecutive phases; when the primary evolves along the RGB at ∼3500 Myr, on the AGB at ∼3650 Myr, and when the secondary is on the RGB at ∼4100 Myr. Left and middle panels: inner semimajor axis and eccentricity as a function of time. Right panel: circularisation of the inner orbit in the final stages before the mass transfer. Left panel: we have overplotted in dashed grey the widening of the inner orbit if only stellar winds would act upon it. The initial conditions of this system are: m₁ = 1.42 M_⊙, m₂ = 1.36 M_⊙, m₃ = 0.70 M_⊙, i = 70.9°, a_in = 3057 R_⊙, e_in = 0.86, g_in = 1.30 rad, a_out = 116 551 R_⊙, e_out = 0.70, g_out = −1.99 rad.