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Galactic Cosmic Rays (GCRs) are mainly protons confined in the galacticmagnetic field to form an isotropic flux inside the galaxy. Before reaching theEarth orbit they enter the Heliosphere and undergo diffusion, convection,magnetic drift and adiabatic energy loss. The result is a reduction ofparticles flux at low energy (below 10 GeV), called solar modulation. Werealized a quasi time-dependent 2D Stochastic Simulation of Solar Modulationthat is able to reproduce CR spectra once known the Local Interstellar Spectrum(LIS). We were able to estimate the different behaviors associated to thepolarity dependence of the Heliospheric modulation for particles as well as forantiparticles. We show a good agreement with the antiproton/proton ratiomeasured by AMS-01, Pamela, BESS, Heat and Caprice and we performed aprediction for the AMS-02 Experiment.

Proton and antiproton modulation in the heliosphere for different solar conditions and AMS-02 measurements prediction