Simulations of the rapid modification of radiation belt electron distributions through large amplitude oblique whistler wave-particle interactions

Details Simulations of the rapid modification of radiation belt electron distributions through large amplitude oblique whistler wave-particle interactions Simulations of the rapid modification of radiation belt electron distributions through large amplitude oblique whistler wave-particle interactions

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm13b2046k&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SM13B-2046

Physics

Plasma Physics

[2774] Magnetospheric Physics / Radiation Belts, [7807] Space Plasma Physics / Charged Particle Motion And Acceleration, [7867] Space Plasma Physics / Wave/Particle Interactions

Scientific paper

With the recent discovery of very large amplitude whistler mode waves in the Earth's radiation belts, there has been a renewal of focused investigation into the mechanisms of radiation belt particle energization and transport; the question of the validity of quasi-linear versus full nonlinear treatment of wave-particle interactions remains a topic of active debate. We present the results of relativistic test particle simulations exploring the effect of large amplitude oblique whistler mode waves on substorm injected energetic electron distributions. Our study employs a large parallel relativistic test particle simulation capable of tracking the individual trajectories of a large ensemble of particles through interactions with oblique whistler mode waves along a single flux tube. The background field is scaled to match the Earth's dipole field, allowing the tracking of the loss of energetic particles to the atmosphere. Initial results indicate that particles occupying a large region of phase space undergo the usual stochastic evolution in both energy and pitch angle, while small regions of phase space are subject to either rapid energization or scattering, or a combination of energization and scattering. Using input particle distributions modeled on LANL energetic electron flux data and available radiation belt pitch angle distributions, we will attempt to characterize what may be observed by energetic particle detectors in equatorial orbit through the radiation belts and at the footpoints of radiation belt magnetic field lines, e.g., what may be expected by the RBSP and BARREL investigations.

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