Radiation belt electron flux variability during three CIR-driven geomagnetic storms

Details Radiation belt electron flux variability during three CIR-driven geomagnetic storms Radiation belt electron flux variability during three CIR-driven geomagnetic storms

Jul 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009jastp..71.1145l&link_type=abstract

Journal of Atmospheric and Solar-Terrestrial Physics, Volume 71, Issue 10-11, p. 1145-1156.

Physics

2

High Speed Solar Wind, Magnetic Storms, Radiation Belts, Wave-Particle Interactions

Scientific paper

Coronal holes produce high speed solar wind streams (HSS) that subsequently interact with the slower downstream solar wind forming co-rotating interaction regions (CIRs). The CIR/HSS combination drives geomagnetic storms that have a weak to moderate signature in Dst. We simulate the behavior of relativistic (976 keV) electrons in the outer radiation belt and the slot region (2[less-than-or-equals, slant]L[less-than-or-equals, slant]7) during three CIR-driven storms associated with three consecutive rotations of a coronal hole that occurred just after solar maximum during June-August 1991. We use a 1d radial diffusion model (RADICAL) with losses due to pitch-angle scattering by plasmaspheric hiss. The losses are expressed through the electron lifetime calculated using the PADIE code driven by a global Kp-dependent model of plasmaspheric hiss intensity and fpe/fce. The outer boundary condition is time and energy-dependent and derived from observations. The model reproduces the observed flux at L=5 to within about a factor of 3 suggesting that flux levels are well-described by radial diffusion to and from the outer boundary. At L=3.5 and 4, the model overestimates the flux decay rates. This results in the observed flux exceeding the model flux, by up to a factor of 5 at L=4 and by up to a factor of 8 at L=3.5, by the end of the recovery phase. Comparison with model results from a geomagnetically quieter interval suggest that the underestimation in flux may be due to the lack of representation of local wave acceleration in the model.

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