On the radial distribution of Galactic cosmic rays

TL;DR

This paper models non-linear cosmic ray propagation in the Galaxy, explaining observed variations in CR density and spectral softening with distance from the Galactic Center, challenging standard uniform diffusion assumptions.

Contribution

It introduces a non-linear CR propagation model with self-generated turbulence, accounting for spatial CR distribution and spectral changes based on source and magnetic field distributions.

Findings

CR density profile matches observations with non-linear model

Spectral softening explained by self-generated turbulence

Challenges standard uniform diffusion assumptions

Abstract

The spectrum and morphology of the diffuse Galactic gamma-ray emission carries valuable information on cosmic ray (CR) propagation. Recent results obtained by analyzing Fermi-LAT data accumulated over seven years of observation show a substantial variation of the CR spectrum as a function of the distance from the Galactic Center. The spatial distribution of the CR density in the outer Galaxy appears to be weakly dependent upon the galactocentric distance, as found in previous studies as well, while the density in the central region of the Galaxy was found to exceed the value measured in the outer Galaxy. At the same time, Fermi-LAT data suggest a gradual spectral softening while moving outward from the center of the Galaxy to its outskirts. These findings represent a challenge for standard calculations of CR propagation based on assuming a uniform diffusion coefficient within the Galactic volume. Here we present a model of non-linear CR propagation in which transport is due to particle scattering and advection off self-generated turbulence. We find that for a realistic distribution of CR sources following the spatial distribution of supernova remnants and the space dependence of the magnetic field on galactocentric distance, both the spatial profile of CR density and the spectral softening can easily be accounted for.