Superthermal electrons and Bernstein waves in Jupiter's inner magnetosphere

Details Superthermal electrons and Bernstein waves in Jupiter's inner magnetosphere Superthermal electrons and Bernstein waves in Jupiter's inner magnetosphere

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980jgr....85.6729b&link_type=abstract

Journal of Geophysical Research, vol. 85, Dec. 1, 1980, p. 6729-6742.

Physics

10

Harmonic Generations, High Energy Electrons, Jupiter Atmosphere, Magnetospheric Instability, Planetary Magnetospheres, Atmospheric Models, Magnetospheric Electron Density, Power Spectra, Ray Tracing

Scientific paper

A theoretical model for generation of banded electrostatic emissions by low density, superthermal electrons is developed for application to Jupiter's magnetosphere. The model employs a power law form for the energy dependence and a loss cone pitch angle distribution of the superthermals to drive convective instability of Bernstein modes. A direct correspondence between spectral features of the 3/2 band and resonant superthermal electrons is found. The concept of a critical flux of resonant electrons able to provide 10 e-foldings of electric field amplification yields an explicit relation in terms of the background thermal electron pressure. This result is used to construct a theoretical/empirical model of thermal electron density and temperature from 6-20 Jupiter radii in the Jovian magnetosphere which suggests that the electron temperature is less than the ion temperature which is approximately equal to 10 times the electron temperature in this region. Finally, wave ray paths are computed for propagation in the magnetic equator and in the magnetic meridional plane of a dipole magnetic field. These ray paths suggest that intense wave activity is tightly confined to a small latitudinal extent, less than + or - approximately 4 deg, about the magnetic equator.

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