Speaker
Description
The propagation of Galactic cosmic rays (GCRs) is influenced by both the Galactic magnetic field and anisotropic diffusion processes. To accurately model this propagation near the solar system, we employ a non-uniform grid method. This method allows for high-resolution simulations of GCR propagation in the solar system's vicinity while maintaining computational efficiency on larger scales. The spatially dependent diffusion tensor is incorporated to account for the anisotropic nature of GCR diffusion, which varies with spatial position and magnetic field structure. Additionally, we consider the effect of nearby sources on GCR propagation, which may influence the observed anisotropies. Our results demonstrate that this method accurately reproduces the observed anisotropies in the TeV to PeV energy range, offering a more precise understanding of GCR diffusion and anisotropy. By refining the description of cosmic ray diffusion with high-resolution grid points, we provide a more precise understanding of GCR propagation and anisotropy, bringing us closer to identifying the sources of these particles.
