Formation of an Accelerated Ion Population by Electromagnetic, non-MHD,Finite-size, Fast-mode Shocks.

Details Formation of an Accelerated Ion Population by Electromagnetic, non-MHD,Finite-size, Fast-mode Shocks. Formation of an Accelerated Ion Population by Electromagnetic, non-MHD,Finite-size, Fast-mode Shocks.

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh33a1192r&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH33A-1192

Physics

7514 Energetic Particles (2114), 2114 Energetic Particles, Heliospheric (7514), 2118 Energetic Particles, Solar

Scientific paper

Solar Energetic Particles form high energy tails which affect the geophysical environment and impose a significant hazard for manned space exploration.An important site for their energization is related to propagating shocks,which assume a variety of shapes and often appear in tandem. Although most of the numerical investigations address the energization mechanisms through diffusion-like approach, basically it is (a) kinetic in nature, (b) occurs often over small spatial scales, and (c) is very sensitive to the details of the shock fields and seed population. We construct a self-consistent, non-MHD, electromagnetic configuration, made from a solitary shock or combined from two propagating shocks, perform an explicit integration of particle trajectories with detailed focus on their initial conditions, and investigate the plausibility of thermal source for the energized population. It is found that:(1) the energization of ions for low Mach numbers ( ˜2) as observed for emerging shocks close to Sun depends crucially on the narrow size of the shock, (2) the gyration phase and the obliqueness of the particle flow direction with respect to the shock normal determines the seed population;(3) the acceleration by shock surfing becomes a prerequisite for scattering,reflection and additional energization due to multiple shock crossing.

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