Datensatz

Zusammenfassung

Both resonant and non-resonant instabilities are responsible for the self-generation of hydromagnetic waves in the precursor of collisionless shock waves. These waves facilitate the scattering of relativistic particles necessary for the diffusive acceleration of cosmic rays. 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, and calculate the transport properties of test-particles in a snapshot of the resultant field. It is shown that even for modest field amplification that sub-Bohm diffusion can be achieved 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.