[en] We construct theoretical models of interstellar radiative shocks, with special attention to the transfer of ionizing radiation. These models are ''self-consistent'' in the sense that the emergent ionizing radiation (the UV precursor) is coupled with the ionization state of H, He, and the metals in the preshock gas. For shock velocities upsilon/sub s/> or =110 km s^-1 the shocks generate sufficient UV radiation for complete preionization of H and He (to He⁺). At lower velocities the preionization can be much smaller, with important consequences for the cooling function, the shock structure, and the emission. For models with 40 km s^-1< or =upsilon/sub s/< or =130 km s^-1 we tabulate the intensities of the strongest emission lines in the UV, optical, and infrared, as well as postshock column densities of metal ions potentially observable by UV absorption spectroscopy. Possible applications to supernova remnants and high-velocity interstellar gas are assessed