An emission mechanism for the Io-independent Jovian decameter radiation

Details An emission mechanism for the Io-independent Jovian decameter radiation An emission mechanism for the Io-independent Jovian decameter radiation

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...230..261g&link_type=abstract

Astrophysical Journal, Part 1, vol. 230, May 15, 1979, p. 261-273. Research supported by the University of Maryland and NASA.

Astronomy and Astrophysics

Astrophysics

4

Astronomical Models, Decametric Waves, Jupiter (Planet), Planetary Radiation, Radio Emission, Io, Jupiter Atmosphere, Magnetic Storms, Planetary Magnetic Fields, Refraction, Spectrum, Io, Radiation, Jupiter, Satellites, Flux, Radio, Plasmas, Electrons, Pioneer 10, Pioneer 11, Decameter Waves, Magnetic Fields, Electromagnetic Fields

Scientific paper

A theory of the Io-independent decameter radiation is developed. The radiation results from excitation of the electromagnetic loss-cone instability by keV electrons, stably trapped near L = 6. The radiation is excited in band III of the extraordinary mode. When the effects of refraction are estimated, it is shown that above 10 MHz radiation is beamed into the equatorial plane in a wide, but thin, conical sheet. When the instability analysis is coupled with one of the octopole models of the Jovian magnetic field, the maximum convective growth of the instability occurs in the directions of the non-Io A, B, and C sources. The shape of the peak radio flux frequency spectrum is found to be a consequence of the loss-cone shape of the electron distribution function.

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