Structure of Cosmic Ray-modified Perpendicular Shocks

Details Structure of Cosmic Ray-modified Perpendicular Shocks Structure of Cosmic Ray-modified Perpendicular Shocks

2009-12-09

arxiv.org/abs/0912.1784v1

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

12 pages, 1 Fig

Scientific paper

Kinetic diffusion of cosmic rays ahead of perpendicular shocks induces charge non-neutrality, which is mostly, yet not completely, screened by the bulk plasma via polarization drift current. Hydrodynamic shear instabilities as well as modified Buneman instability of the polarization current generate the turbulence necessary for a Fermi-type acceleration. Thus, similar to the case of parallel shocks, in perpendicular shocks the diffusing cosmic rays generate unstable plasma currents that in turn excite turbulence. This allows a self-consistent evolution of a shock-cosmic rays system. In the kinetic regime of the modified Buneman instability, electrons may be heated in the cosmic ray precursor.

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