HR: 0800h
AN: SM41A-1175    [Abstracts]
TI: Precipitated Fluxes of Radiation Belt Electrons via Injection of Whistler-Mode Waves
AU: * Kulkarni, P
EM: pxk161@stanford.edu
AF: STAR Laboratory Stanford University, 350 Serra Mall, Stanford, CA 94305
AU: Inan, U S
EM: inan@stanford.edu
AF: STAR Laboratory Stanford University, 350 Serra Mall, Stanford, CA 94305
AU: Bell, T F
EM: bell@nova.stanford.edu
AF: STAR Laboratory Stanford University, 350 Serra Mall, Stanford, CA 94305
AB: Inan et al. (U.S. Inan et al., Controlled precipitation of radiation belt electrons, Journal of Geophysical Research-Space Physics, 108 (A5), 1186, doi: 10.1029/2002JA009580, 2003.) suggested that the lifetime of energetic (a few MeV) electrons in the inner radiation belts may be moderated by in situ injection of whistler mode waves at frequencies of a few kHz. We use the Stanford 2D VLF raytracing program (along with an accurate estimation of the path-integrated Landau damping based on data from the HYDRA instrument on the POLAR spacecraft) to determine the distribution of wave energy throughout the inner radiation belts as a function of injection point, wave frequency and injection wave normal angle. To determine the total wave power injected and its initial distribution in k-space (i.e., wave-normal angle), we apply the formulation of Wang and Bell ( T.N.C. Wang and T.F. Bell, Radiation resistance of a short dipole immersed in a cold magnetoionic medium, Radio Science, 4 (2), 167-177, February 1969) for an electric dipole antenna placed at a variety of locations throughout the inner radiation belts. For many wave frequencies and wave normal angles the results establish that most of the radiated power is concentrated in waves whose wave normals are located near the resonance cone. The combined use of the radiation pattern and ray-tracing including Landau damping allows us to make quantitative estimates of the magnetospheric distribution of wave power density for different source injection points. We use these results to estimate the number of individual space-based transmitters needed to significantly impact the lifetimes of energetic electrons in the inner radiation belts. Using the wave power distribution, we finally determine the energetic electron pitch angle scattering and the precipitated flux signatures that would be detected.
DE: 2716 Energetic particles: precipitating
DE: 2730 Magnetosphere: inner
DE: 2774 Radiation belts
SC: SPA-Magnetospheric Physics [SM]
MN: Fall Meeting 2005