2008/02/01 by Brian Reville, B. Reville, S. P. O’Sullivan +3 · 4 citations
Physics and Astronomy · #Acceleration #Astrophysics #Astrophysics and Cosmic Phenomena #Atomic physics #Classical mechanics #Computational physics #Cosmic ray #Excited state #Gamma-ray bursts and supernovae #Gyroradius #Instability #Magnetic field #Magnetohydrodynamic turbulence #Magnetohydrodynamics #Mechanics #Particle acceleration #Physics #Quantum mechanics #Shock wave #Solar and Space Plasma Dynamics #Streaming instability #Supernova #Turbulence #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2008.13059.x
8 pages, 8 figures, accepted for publication in MNRAS
arxiv created 2008/02/01 · openalex publication_date 2008/03/11 · arxiv updated 2009/12/01 · openalex created_date 2020/11/23 · openalex updated_date 2026/08/05
The process of diffusive shock acceleration relies on the efficacy with which hydromagnetic waves can scatter charged particles in the precursor of a shock. The growth of self-generated waves is driven by both resonant and non-resonant processes. We perform high-resolution magnetohydrodynamic simulations of the non-resonant cosmic ray driven instability, in which the unstable waves are excited beyond the linear regime. In a snapshot of the resultant field, particle transport simulations are carried out. The use of a static snapshot of the field is reasonable given that the Larmor period for particles is typically very short relative to the instability growth time. The diffusion rate is found to be close to, or below, the Bohm limit for a range of energies. This provides the first explicit demonstration that self-excited turbulence reduces the diffusion coefficient and has important implications for cosmic-ray transport and acceleration in supernova remnants.