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Physical conditions in dense and cold regions of interstellar clouds favourthe formation of ice mantles on the surfaces of interstellar grains. It ispredicted that most of the gaseous species heavier than H2 or He will adsorbonto the grains and will disappear from the gas-phase, changing its chemistry,within 10^9/n_H years. Nonetheless, many molecules in molecular clouds are notcompletely depleted in timescales of 10^5 yr. Several speculative mechanismshave been proposed to explain why molecules stay in the gas phase, but up tonow none are fully convincing. At the same time, these mechanisms are notmutually exclusive and we can still explore the effects of other possibleprocesses. We speculate on the consequences of H2 coating of grains on theevaporation rates of adsorbed species. More experiments and simulations areneeded to calculate the evaporation rate Eevap(X-H2).

Effects of H2 coating of grains on depletion of molecular species