The distribution of metals across a range of environments, from the dwarf galaxies to the local interstellar medium (ISM), shows an isotope-by-isotope dispersion which is often orders of magnitude in excess of that expected from observational uncertainty alone. Such intrinsic dispersions hint at very important underlying physics which cannot be captured by the traditional homogeneous approach to galactic chemical evolution, including, for example, the feedback coupling efficiency between supernovae and the ISM. The computational expense associated with fully hydrodynamical and gravitational N-body approaches limits their application to unique / targeted cases. Here, we present a fast and efficient hybrid approach to tracking the temporal evolution of isotopic abundance patterns, accounting for the inhomogeneous structure of the ISM, as well as the mass and metallicity-dependent nature of supernovae feedback. Examples of the power of such an approach will be drawn from the modeling of the local ISM, the Milky Way’s stellar halo, and Local Group dwarf galaxies.