Building the Galactic magnetic halo
The Cosmic Ray (CR) physics has entered a new era driven by high precision measurements coming from direct detection (especially AMS-02 and PAMELA) as well as gamma-ray observations (Fermi-LAT) which requires the development of more refined models for the CR acceleration and propagation. In this talk I will present a model for the generation of the Galactic magnetic halo where Cosmic Rays propagate. The magnetic halo is builded by two separated processes: 1) the large-scale magnetic turbulence generated into the galactic plane and advected away from it while cascading towards smaller scales and 2) the small-scale turbulence self-generated by CRs that escape from the Galaxy. The decay process of large scale turbulence naturally predicts a magnetic halo size of ~ 2-5 kpc, as required by the majority of CR models. Moreover, the interplay between these two processes can explain the break observed in the CR spectrum at ~300 GV by AMS-02.