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

E Fiandrini,B Khiali,A Reina Conde,B Bertucci,F Donnini,N Tomassetti,M Graziani

doi:10.1103/physrevd.104.023012

Abstract

Galactic cosmic rays (CRs) inside the heliosphere are affected by solar modulation. To investigate this phenomenon and its underlying physical mechanisms, we have performed a data-driven analysis of the temporal dependence of the CR proton flux over the solar cycle. The modulation effect was modeled by means of stochastic simulations of cosmic particles in the heliosphere. The model were constrained using measurements of CR protons made by AMS-02 and PAMELA experiments on monthly basis from 2006 to 2017. With a global statistical analysis of these data, we have determined the key model parameters governing CR diffusion, its dependence on the particle rigidity, and its evolution over the solar cycle. Our results span over epochs of solar minimum, solar maximum, as well as epochs with magnetic reversal and opposite polarities. Along with the evolution of the CR transport parameters, we study their relationship with solar activity proxies and interplanetary parameters. We find that the rigidity dependence of the parallel mean free path of CR diffusion shows a remarkable time dependence, indicating a long-term variability in the interplanetary turbulence that interchanges across different regimes over the solar cycle. The evolution of the diffusion parameters show a delayed correlation with solar activity proxies, reflecting the dynamics of the heliospheric plasma, and distinct dependencies for opposite states of magnetic polarity, reflecting the influence of charge-sign dependent drift in the CR modulation.

Highlights

Galactic cosmic rays (CRs) are high-energy charged particles produced by astrophysical sources, distributed in our Galaxy, which travel through the interstellar medium and arrive at the boundary of the nearby region to Earth, where the Sun’s activity dominates: the so-called heliosphere
We find that the rigidity dependence of the parallel mean free path of CR diffusion shows a remarkable time dependence, indicating a long-term variability in the interplanetary turbulence that interchanges across different regimes over the solar cycle
We found that the agreement between best-fit model and the measurements on the fluxes of CR protons was, in general, very good for all the datasets and over the whole rigidity range

Summary

Introduction

Galactic cosmic rays (CRs) are high-energy charged particles produced by astrophysical sources, distributed in our Galaxy, which travel through the interstellar medium and arrive at the boundary of the nearby region to Earth, where the Sun’s activity dominates: the so-called heliosphere. CRs travel against the expanding solar wind (SW) and interact with the turbulent heliospheric magnetic field (HMF) [1]. They are subjected to basic transport processes such as convection, diffusion, and adiabatic energy losses. They are subjected to the gradient-curvature drifts in the large-scale HMF and to the effects of the heliospheric current sheet (HCS).

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