Evolution of D/H ratio enrichment for our nominal disk. These profiles allow an important D/H ratio diversity in the chondrite formation region. They explain the values measured in the different chondrite families from their formation location. These inferred formation locations are also compatible with the water abundances of chondrites, with OCs and CRs containing less water (hence probably forming closer to the Sun) than CMs and CIs. The exact distance relative to the Sun is not important since the model is scalable with Ṁ_infall. The D/H ratios in comets, Enceladus, and VSMOW (Earth) are shown for reference. Having f decreasing to low values in the cometary region at late times is an artifact of our disk cooling treatment and should be higher with a consistent treatment. Indeed, when the temperature drops below the water condensation point, we keep evolving f, letting it continue to drop, while it should be fixed at the value reached when the water became isolated from gas by freezing.