Typical evolution of the binary that becomes an IMXB and ends up as a merging NS-BH in Model 1. The timescale (in Myr) is shown on the left side of the panel, the masses (in M_⊙) are marked next to the stars they refer to, and the orbital separation (a in R_⊙) and eccentricity (e) of the system at a given stage of the evolution are shown on the right side of the panel. The acronyms on the figure are the same as in Fig. C.1.