J. C. Higdon^{1}, R. E. Lingenfelter^{2}^{1}Claremont McKenna College, Claremont, California, USA^{2}University of California, San Diego, La Jolla, California, USA

We have constructed a Monte Carlo simulation program for the space and time dependent distribution of Galactic supernovae, as a source of both shock energy and particles for cosmic ray acceleration, based on a wide variety of recent astronomical observations and theory. From these simulated distributions of discrete sources, we them determine the form and variance of the expected local cosmic ray path length distribution, assuming a range of effective diffusion mean free paths. These are compared to currently assumed path length distributions and their implications for local cosmic ray abundances are discussed.