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We report on laboratory measurements of molecular hydrogen formation andrecombination on an olivine slab as a function of surface temperature underconditions relevant to those encountered in the interstellar medium. On thebasis of our experimental evidence, we recognize that there are two mainregimes of H coverage that are of astrophysical importance; for each of them weprovide an expression giving the production rate of molecular hydrogen ininterstellar clouds.

Efficiency of Molecular Hydrogen Formation on Silicates