We report on laboratory measurements of molecular hydrogen formation a
nd recombination on an olivine slab as a function of surface temperatu
re under conditions relevant to those encountered in the interstellar
medium. On the basis of our experimental evidence, we recognize that t
here are two main regimes of H coverage that are of astrophysical impo
rtance; for each of them we provide an expression giving the productio
n rate of molecular hydrogen in interstellar clouds.