Non-linear diffusion of cosmic rays escaping from supernova remnants - I. The effect of neutrals

TL;DR

This paper models the non-linear diffusion of cosmic rays from supernova remnants, considering ion-neutral damping effects, and finds significant suppression of cosmic ray diffusion near remnants, impacting gamma-ray observations.

Contribution

It introduces a numerical solution for coupled equations of cosmic ray and wave evolution including ion-neutral damping effects in different interstellar medium phases.

Findings

CR streaming instability persists despite ion-neutral damping.

Diffusion suppression extends over tens of parsecs around remnants.

Cosmic ray propagation timescales vary with energy, affecting gamma-ray signals.

Abstract

Supernova remnants are believed to be the main sources of galactic Cosmic Rays (CR). Within this framework, particles are accelerated at supernova remnant shocks and then released in the interstellar medium. The mechanism through which CRs are released and the way in which they propagate still remain open issues. The main difficulty is the high non-linearity of the problem: CRs themselves excite the magnetic turbulence that confines them close to their sources. We solve numerically the coupled differential equations describing the evolution in space and time of the escaping particles and of the waves generated through the CR streaming instability. The warm ionized and warm neutral phases of the interstellar medium are considered. These phases occupy the largest fraction of the disc volume, where most supernovae explode, and are characterised by the significant presence of neutral particles. The friction between those neutrals and ions results in a very effective wave damping mechanism. It is found that streaming instability affects the propagation of CRs even in the presence of ion-neutral friction. The diffusion coefficient can be suppressed by more than a factor of $\sim 2$ over a region of few tens of pc around the remnant. The suppression increases for smaller distances. The propagation of $\approx 10$ GeV particles is affected for several tens of kiloyears after escape, while $\approx 1$ TeV particles are affected for few kiloyears. This might have a great impact on the interpretation of gamma-ray observations of molecular clouds located in the vicinity of supernova remnants.