English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Talk

Cosmic ray transport in non-resonant current driven MHD turbulence

MPS-Authors
/persons/resource/persons30940

Reville,  Brian
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

/persons/resource/persons30680

Kirk,  John G.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

External Ressource
No external resources are shared
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Reville, B., O'Sullivan, S., Duffy, P., & Kirk, J. G. (2007). Cosmic ray transport in non-resonant current driven MHD turbulence. Talk presented at Seventh European Workshop on Collisionless Shocks. Paris, France. 2007-11-07 - 2007-11-09.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0011-7BB2-4
Abstract
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.