Reconciling the diffuse Galactic gamma-ray and the cosmic ray spectra
Abstract
Most of the diffuse Galactic GeV gamma-ray emission is produced via collisions of cosmic ray (CR) protons with ISM protons. As such the observed spectra of the gamma-rays and the CRs should be strongly linked. Recent observations of Fermi-LAT exhibit a hardening of the gamma-ray spectrum at around a hundred GeV, between the Sagittarius and Carina tangents, and a further hardening at a few degrees above and below the Galactic plane. However, standard CR propagation models that assume a time independent source distribution and a location independent diffusion cannot give rise to a spatially dependent CR (and hence gamma-ray) spectral slopes. Here we consider a dynamic spiral arm model in which the distribution of CR sources is concentrated in the (dynamic) spiral arms, and we study the effects of this model on the -decay produced gamma-ray spectra. Within this model, near the Galactic arms the observed gamma-ray spectral slope is not trivially related to the CR injection spectrum and energy dependence of the diffusion coefficient. We find unique signatures that agree with the Fermi-LAT observations. This model also provides a physical explanation for the difference between the local CR spectral slope and the CR slope inferred from the average gamma-ray spectrum.
Cite
@article{arxiv.1701.02746,
title = {Reconciling the diffuse Galactic gamma-ray and the cosmic ray spectra},
author = {Lara Nava and David Benyamin and Tsvi Piran and Nir J. Shaviv},
journal= {arXiv preprint arXiv:1701.02746},
year = {2017}
}
Comments
8 pages, 8 figures, accepted for publication in MNRAS