Cosmic ray transport and anisotropies to high energies

TL;DR

This paper introduces a multi-regime model of the Galactic magnetic field's irregularity spectrum to explain cosmic ray transport, spectrum, and anisotropies, including implications for ultra high energy cosmic rays.

Contribution

It presents a novel three-regime spectral model of the Galactic magnetic field and applies it to cosmic ray transport and anisotropy analysis.

Findings

Model consistent with ISM data

Explains GCR spectrum and anisotropies

Suggests extragalactic UHECRs include radio galaxy protons

Abstract

A model is introduced, in which the irregularity spectrum of the Galactic magnetic field beyond the dissipation length scale is first a Kolmogorov spectrum $k^{-5/3}$ at small scales $\lambda \, = \, 2 \pi/k$ with $k$ the wave-number, then a saturation spectrum $k^{-1}$, and finally a shock-dominated spectrum $k^{-2}$ mostly in the halo/wind outside the Cosmic Ray disk. In an isotropic approximation such a model is consistent with the Interstellar Medium (ISM) data. With this model we discuss the Galactic Cosmic Ray (GCR) spectrum, as well as the extragalactic Ultra High Energy Cosmic Rays (UHECRs), their chemical abundances and anisotropies. UHECRs may include a proton component from many radio galaxies integrated over vast distances, visible already below 3 EeV.