Whistler mode emissions in the Uranian radiation belts

Details Whistler mode emissions in the Uranian radiation belts Whistler mode emissions in the Uranian radiation belts

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987jgr....9215234c&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 92, Dec. 30, 1987, p. 15234-15248.

Astronomy and Astrophysics

Astronomy

33

Magnetospheric Electron Density, Radiation Belts, Radio Emission, Spaceborne Astronomy, Uranus Atmosphere, Whistlers, Particle Flux Density, Plasma Turbulence, Plasma Waves, Propagation Modes, Voyager 2 Spacecraft

Scientific paper

Voyager 2 detected intense whistler mode emissions and fluxes of energetic electrons during the outbound pass through the region of auroral L shells. The observed energetic (E greater than 22 keV) electron distribution, a model warm (E less than 27.5 keV) electron distribution, and the cold plasma density profile deduced by Kurth et al. (1987) are used to calculate the ray path-integrated spatial amplification of whistlers which arrive at Voyager 2 from the magnetic equator. By matching the calculated amplification and the relative gains at different frequencies deduced from the observed whistler power spectrum, the pitch angle anisotropy parameters of the electron distributions are determined to within a fairly narrow range of values. The estimated bounce average pitch angle diffusion coefficient indicates that electrons are on strong diffusion over a wide range in energies. The electron precipitation energy flux is sufficient to produce the observed auroral light emissions.

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