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The ACE-CRIS collaboration has recently released the measurement ofradioactive $^{60}$Fe nuclei abundance in Galactic Cosmic Rays, in the energyrange $\sim 195-500$ MeV per nucleon. We model Cosmic Ray propagation andderive from this measurement the $^{60}$Fe/$^{56}$Fe ratio that is expected inthe sources of Galactic Cosmic Rays. We describe Cosmic Ray origin andtransport within the framework of the disk/halo diffusion model, namely ascenario in which the matter and the Cosmic Ray sources in our Galaxy areconfined to a thin disk, while Cosmic Ray propagation occurs in a much largerhalo with negligible matter density. We solve the Cosmic Ray transport equationaccounting for spallation reactions, decay and ionization losses as well asadvection. We find that the $^{60}$Fe/$^{56}$Fe ratio at the source must bevery close to the value detected in the local Cosmic Ray spectrum at Earth, dueto the fact that spallation reactions are more effective for $^{56}$Fe than for$^{60}$Fe. Such a result could help identify the sources of Galactic CosmicRays.

Impact of transport modelling on the $^{60}$Fe abundance inside Galactic cosmic ray sources