The empirically established initial presence of short-lived radionuclides (SLRs; e.g. 26Al, 53Mn, 60Fe, 182Hf) in the Solar System can both be used to obtain evidence about the timescales of processes in the early Solar System, and to provide constraints on the larger scale environment where our Sun was formed. Many SLRs are believed to have had a stellar origin, and may have either been inherited from the molecular cloud that the Sun was born in, or may have been injected into the proto-solar molecular cloud core just prior to or contemporaneously with its collapse. In particular, recent high-precision measurements of 26Mg (the daughter product of 26Al) in meteorites and their components show that, despite its short half-life of 0.73 Ma, 26Al was present at levels large enough to melt asteroids and planetesimals in the early solar system. In order to use the information available from SLR analysis a good understanding of the transport and distribution of the SLRs in star-forming regions is needed, and we have set out to study these mechanisms using three-dimensional MHD models of star formation that keep track of yields from supernovae and stellar winds via an additional passive scalar transport equation.