Radiation belt modeling of the Oct. 2001 storm

Details Radiation belt modeling of the Oct. 2001 storm Radiation belt modeling of the Oct. 2001 storm

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsm42a..03m&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SM42A-03

Physics

2730 Magnetosphere: Inner, 2753 Numerical Modeling, 2774 Radiation Belts, 2780 Solar Wind Interactions With Unmagnetized Bodies, 7867 Wave/Particle Interactions (2483, 6984)

Scientific paper

We simulate the evolution of phase space distribution function of ring current and radiation belt electrons for energy range from a few hundred eV to a few MeV using the relativistic RAM code [Jordanova and Miyoshi, GRL, 2005], which solves the time-dependent, bounce-averaged kinetic equation for particle drifts, radial diffusion and several loss processes. The loss processes in the RAM model include Coulomb collisions, wave particle interactions, and escaping from dayside magnetopause. In the simulation, the time-dependent particle distributions measured from the MPA and SOPA instruments on the geosynchronous LANL satellites are used as the outer boundary conditions. As the event for simulation study, we have examined the October 2001 magnetic storm [Miyoshi et al., JGR, 2006]. In this study, we report the following two topics; i) the temporal-spatial evolution of whistler mode waves which should have an impact for the acceleration and scattering of the relativistic electrons, ii) the impact of EMIC waves for scattering of energetic electrons. About the first topic, we calculated the growth rate of whistler mode waves and found that the intense whistler mode waves are generated from post-midnight to dawn side outside the plasmapause. The results of this simulation exhibit similar behavior to the statistical distribution of whistler mode chorus waves reported from CRRES observations. About the second topic, we calculated the pitch angle scattering rate of relativistic electrons with EMIC waves using the temporal and spatial distribution of EMIC waves from the RAM-ion calculations [Jordanova et al., JGR, 2006]. The simulation indicated that the significant precipitation into the atmosphere was found at the post-noon side. The precipitation was not seen at the hundred keV electrons but seen only at MeV electrons. The results indicate clearly that EMIC waves have a significant impact on loss of MeV electrons.

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