Inhomogeneous Chemical Evolution of the Galactic Halo

We describe the basic features of a Monte Carlo model specifically designed to follow the inhomogenous chemical evolution of the Galactic halo, taking into account the effects of local enrichment and mixing of the halo gas, and with particular emphasis on elements like Eu produced by r-process nucleosynthesis. We compare our results with spectroscopic data for the chemical composition of metal-poor halo stars and globular clusters like M13, M5, M92, M4, and we infer some constraints on the star formation history of the halo and the rate and mass spectrum of supernovae during the first epoch of Galaxy evolution.