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CO is thought to be a vital building block for prebiotic molecules that arenecessary for life. Thus, understanding where CO existed in a solid phasewithin the solar nebula is important for understanding the origin of life. Wemodel the evolution of the CO snow line in a protoplanetary disk. We find thatthe current observed location of the CO snow line in our solar system, and inthe solar system analogue TW Hydra, cannot be explained by a fully turbulentdisk model. With time-dependent disk models we find that the inclusion of adead zone (a region of low turbulence) can resolve this problem. Furthermore,we obtain a fully analytic solution for the CO snow line radius for late diskevolutionary times. This will be useful for future observational attempts tocharacterize the demographics and predict the composition and habitability ofexoplanets.

On the evolution of the CO snow line in protoplanetary disks