Evaluation of quasi-linear diffusion coefficients for whistler mode waves in a plasma with arbitrary density ratio

Details Evaluation of quasi-linear diffusion coefficients for whistler mode waves in a plasma with arbitrary density ratio Evaluation of quasi-linear diffusion coefficients for whistler mode waves in a plasma with arbitrary density ratio

Mar 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jgra..11003218a&link_type=abstract

Journal of Geophysical Research, Volume 110, Issue A3, CiteID A03218

Physics

Plasma Physics

51

Magnetospheric Physics: Radiation Belts, Magnetospheric Physics: Energetic Particles: Trapped, Magnetospheric Physics: Magnetosphere: Inner, Space Plasma Physics: Wave/Particle Interactions (2483, 6984), Radio Science: Magnetospheric Physics (2700)

Scientific paper

Techniques are presented for efficiently evaluating quasi-linear diffusion coefficients for whistler mode waves propagating according to the full cold plasma index of refraction. In particular, the density ratio ωpe/Ωe can be small, which favors energy diffusion. This generalizes an approach, previously used for high-density hiss and electromagnetic ion cyclotron waves, of identifying (and omitting) ranges of wavenormal angle $\theta$ that are incompatible with cyclotron resonant frequencies ω occurring between sharp cutoffs of the modeled wave frequency spectrum. This requires a detailed analysis of the maximum and minimum values of the refractive index as a function of ω and $\theta$, as has previously been performed in the high-density approximation. Sample calculations show the effect of low-density ratio on the pitch angle and energy diffusion coefficients modeling the effect of chorus waves on radiation belt electrons. The high-density approximation turns out to be quite robust, especially when the upper frequency cutoff is small compared with Ωe. The techniques greatly reduce the amount of computation needed for a sample calculation, while taking into account all resonant harmonic numbers n up to +/-∞.

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