Abstract
There is a growing set of observational data demonstrating that cosmic rays exhibit small-scale anisotropies (5°-30°) with amplitude deviations lying between 0.01-0.1 per cent that of the average cosmic ray flux. A broad range of models have been proposed to explain these anisotropies ranging from finite-scale magnetic field structures to dark matter annihilation. The standard diffusion transport methods used in cosmic ray propagation do not capture the transport physics in a medium with finite-scale or coherent magnetic field structures. Here, we present a Monte Carlo transport method, applying it to a series of finite-scale magnetic field structures to determine the requirements of such fields in explaining the observed cosmic ray, small-scale anisotropies.
Original language | English |
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Pages (from-to) | 3497-3510 |
Number of pages | 14 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 500 |
Issue number | 3 |
DOIs | |
State | Published - Jan 1 2021 |
Externally published | Yes |
Funding
This work was supported by the U.S. Department of Energy through the Los Alamos National Laboratory. Los Alamos National Laboratory is operated by Triad National Security, LLC, for the National Nuclear Security Administration of U.S. Department of Energy (contract no. 89233218CNA000001) This research was supported in part by the National Science Foundation under grant no. NSF PHY-1748958 and by NASA Astrophysics Theory Program grant 80NSSC20K0507.
Funders | Funder number |
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National Science Foundation | PHY-1748958 |
U.S. Department of Energy | |
Directorate for Mathematical and Physical Sciences | 1748958 |
National Aeronautics and Space Administration | 80NSSC20K0507 |
National Nuclear Security Administration | 89233218CNA000001 |
Los Alamos National Laboratory |
Keywords
- Astroparticle physics
- Cosmic rays
- ISM: Magnetic fields