Speaker
Description
The spatial diffusion of energetic particles in a magnetic field composed of a large-scale background and a small-scale turbulent component should be expected to be anisotropic. While such anisotropic diffusion has been known for quite a while in first-principle plasma physics and while it is required for an understanding of the transport of cosmic rays in the heliosphere or close to supernova remnants, only in recent years it has also become of particular interest for the modeling of Galactic cosmic ray (GCRs) transport in the Milky Way in the context of their residence time and their (local) energy spectra. The large-scale spatial distribution of GCRs is shaped by an anisotropic diffusion in the Galactic magnetic field which should directly affect both the diffuse gamma-ray and the neutrino emission.
In this talk, I will demonstrate that an anisotropic diffusive transport of GCRs in the Milky Way has an imprint on the all-sky gamma-ray emission in the GeV to TeV range. For this we calculate the CR distribution in the Milky Way considering anisotropic transport using the public CRPropa framework and estimate the line-of-sight emission with the HERMES package. Finally, I will discuss the feasibility of gamma-ray observations to constrain not only the parameters of such anisotropic transport but also the structure of the Galactic magnetic field.
