Cosmic ray transport and anisotropies

TL;DR

This paper proposes that the large-scale anisotropy of cosmic rays at around 10 TeV can be explained by a modified Compton-Getting effect influenced by supernova remnants, with specific predictions about energy dependence.

Contribution

It introduces a novel explanation for cosmic ray anisotropy involving a modified Compton-Getting effect in supernova remnant environments, incorporating turbulence and stellar wind interactions.

Findings

Anisotropy amplitude varies with energy, being smaller at lower and higher energies.

Propagation modeled with Kolmogorov turbulence and stellar wind interactions.

Predicts an optimal energy scale for detecting cosmic ray anisotropy.

Abstract

We show that the large-scale cosmic ray anisotropy at ~10 TeV can be explained by a modified Compton-Getting effect in the magnetized flow field of old supernova remnants. This approach suggests an optimum energy scale for detecting the anisotropy. Two key assumptions are that propagation is based on turbulence following a Kolmogorov law and that cosmic ray interactions are dominated by transport through stellar winds of the exploding stars. A prediction is that the amplitude is smaller at lower energies due to incomplete sampling of the velocity field and also smaller at larger energies due to smearing.