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Galactic cosmic rays (CRs) inside the heliosphere are affected by solarmodulation. To investigate this phenomenon and its underlying physicalmechanisms, we have performed a data-driven analysis of the temporal dependenceof the CR proton flux over the solar cycle. The modulation effect was modeledby means of stochastic simulations of cosmic particles in the heliosphere. Themodel were constrained using measurements of CR protons made by AMS-02 andPAMELA experiments on monthly basis from 2006 to 2017. With a globalstatistical analysis of these data, we have determined the key model parametersgoverning CR diffusion, its dependence on the particle rigidity, and itsevolution over the solar cycle. Our results span over epochs of solar minimum,solar maximum, as well as epochs with magnetic reversal and oppositepolarities. Along with the evolution of the CR transport parameters, we studytheir relationship with solar activity proxies and interplanetary parameters.We find that the rigidity dependence of the parallel mean free path of CRdiffusion shows a remarkable time dependence, indicating a long-termvariability in the interplanetary turbulence that interchanges across differentregimes over the solar cycle. The evolution of the diffusion parameters show adelayed correlation with solar activity proxies, reflecting the dynamics of theheliospheric plasma, and distinct dependencies for opposite states of magneticpolarity, reflecting the influence of charge-sign dependent drift in the CRmodulation.

Numerical modeling of cosmic rays in the heliosphere: Analysis of proton data from AMS-02 and PAMELA