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It is thought that the Moon accreted from the protolunar disk that wasassembled after the last giant impact on Earth. Due to its high temperature,the protolunar disk may act as a thermochemical reactor in which the materialis processed before being incorporated into the Moon. Outstanding issues likedevolatilisation and istotopic evolution are tied to the disk evolution,however its lifetime, dynamics and thermodynamics are unknown. Here, wenumerically explore the long term viscous evolution of the protolunar diskusing a one dimensional model where the different phases (vapor and condensed)are vertically stratified. Viscous heating, radiative cooling, phasetransitions and gravitational instability are accounted for whereas Moon saccretion is not considered for the moment. The viscosity of the gas, liquidand solid phases dictates the disk evolution. We find that (1) the vaporcondenses into liquid in about 10 years, (2) a large fraction of the disk massflows inward forming a hot and compact liquid disk between 1 and 1.7 Earth sradii, a region where the liquid is gravitationally stable and can accumulate,(3) the disk finally solidifies in 1000 to 100,000 years. Viscous heating isnever balanced by radiative cooling. If the vapor phase is abnormally viscous,due to magneto-rotational instability for instance, most of the disk volatilecomponents are transported to Earth leaving a disk enriched in refractoryelements. This opens a way to form a volatile-depleted Moon and would suggestthat the missing Moon s volatiles are buried today into the Earth. The diskcooling timescale may be long enough to allow for planet-disk isotopicequilibration. However large uncertainties on the disk physics remain becauseof the complexity of its multi-phased structure.

Evolution of the protolunar disk: dynamics, cooling timescale and implantation of volatiles onto the Earth