Galactic cosmic-ray propagation in the light of AMS-02: I. Analysis of protons, helium, and antiprotons

TL;DR

This study uses recent AMS-02 cosmic-ray data to constrain Galactic magnetic turbulence and propagation parameters, employing advanced statistical methods to analyze proton, helium, and antiproton spectra.

Contribution

It introduces a comprehensive Bayesian analysis of cosmic-ray propagation parameters using AMS-02 data, with novel constraints on magnetic turbulence and propagation effects.

Findings

Magnetic turbulence spectral index constrained to δ=0.30 with uncertainties.

Reacceleration velocity determined to be 25±2 km/s, dependent on solar modulation assumptions.

Convection and reacceleration effects are degenerate and not individually well-constrained.

Abstract

We present novel constraints on cosmic-ray propagation in the Galaxy using the recent precise measurements of proton and helium spectra from AMS-02, together with preliminary AMS-02 data on the antiproton over proton ratio. To explore efficiently the large (up to eleven-dimensional) parameter space we employ the nested-sampling algorithm as implemented in the \textsc{MultiNest} package, interfaced with the \textsc{Galprop} code to compute the model-predicted spectra. We use VOYAGER proton and helium data, sampling the local inter-stellar spectra, to constrain the solar modulation potential. We find that the turbulence of the Galactic magnetic field is well constrained, i.e., $\delta=0.30^{+0.03}_{-0.02}(stat)^{+0.10}_{-0.04}(sys)$, with uncertainties dominated by systematic effects. Systematic uncertainties are determined checking the robustness of the results to the minimum rigidity cut used to fit the data (from 1 GV to 5 GV), to the propagation scenario (convection vs no-convection), and to the uncertainties in the knowledge of the antiproton production cross section. Convection and reaccelaration are found to be degenerate and not well-constrained singularly when using data above 5 GV. Using data above 1 GV reacceleration is required, $v_{\rm A}=25\pm2$km/s, although this value might be significantly affected by the low energy systematic uncertainty in the solar modulation. In a forthcoming companion paper, we investigate the constraints imposed by AMS-02 measurements on lithium, boron, and carbon.