Effects of H_2 coating of grains on depletion

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Physical conditions in dense and cold regions of interstellar clouds favor the formation of ice mantles on the surfaces of interstellar grains. It is thought that most of the gaseous species heavier than H_2 will adsorb onto the grains and will disappear from the gas-phase, changing its chemistry, within ˜10^9/n_H years, where n_H is the total hydrogen number density. Nonetheless, many molecules in dense cores in molecular clouds are not completely depleted in timescales of 10^5 yrs. Several speculative mechanisms have been proposed to explain why molecules stay in the gas phase, but up to now none are fully convincing. At the same time, these mechanisms are not exclusive and we can still explore the effects of other possible processes. We speculate on the consequences of H_2 coating of grains on the evaporation rates of adsorbed species. More experiments and simulations are needed to calculate the evaporation rate Eevap(X-H_2). A simplified experiment could be H_2 adsorption on various types of pure ice (H_2O, NH_3, SO, SO_2, H_2CO, ...) to estimate the H_2-X interaction potential.

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