Fickian and non-Fickian diffusion of cosmic rays
| Autor: | Graeme R. Sarson, Anvar Shukurov, A. P. Snodin, Luiz Felippe S. Rodrigues |
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| Rok vydání: | 2019 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics Turbulence FOS: Physical sciences Energy flux Astronomy and Astrophysics 01 natural sciences Fick's laws of diffusion 010305 fluids & plasmas Computational physics Magnetic field Space and Planetary Science 0103 physical sciences Magnetohydrodynamics Test particle Diffusion (business) Astrophysics - High Energy Astrophysical Phenomena Anisotropy 010303 astronomy & astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 487:975-980 |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stz1354 |
| Popis: | Fluid approximations to cosmic ray (CR) transport are often preferred to kinetic descriptions in studies of the dynamics of the interstellar medium (ISM) of galaxies, because they allow simpler analytical and numerical treatments. Magnetohydrodynamic (MHD) simulations of the ISM usually incorporate CR dynamics as an advection-diffusion equation for CR energy density, with anisotropic, magnetic field-aligned diffusion with the diffusive flux assumed to obey Fick's law. We compare test-particle and fluid simulations of CRs in a random magnetic field. We demonstrate that a non-Fickian prescription of CR diffusion, which corresponds to the telegraph equation for the CR energy density, can be easily calibrated to match the test particle simulations with great accuracy. In particular, we consider a random magnetic field in the fluid simulation that has a lower spatial resolution than that used in the particle simulation to demonstrate that an appropriate choice of the diffusion tensor can account effectively for the unresolved (subgrid) scales of the magnetic field. We show that the characteristic time which appears in the telegraph equation can be physically interpreted as the time required for the particles to reach a diffusive regime and we stress that the Fickian description of the CR fluid is unable to describe complex boundary or initial conditions for the CR energy flux. 6 pages, 5 figures. Accepted for publication in MNRAS |
| Databáze: | OpenAIRE |
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