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

Jul 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978stin...7831027g&link_type=abstract

Unknown

Physics

Electromagnetic Radiation, Emission, Io, Jupiter (Planet), Planetary Radiation, Distribution Functions, Electron Distribution, Emission, Magnetic Fields, Power Spectra, Radio Bursts

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 3 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 (Psi approximately equals 80 degrees). When the instability analysis is coupled with one of the octupole 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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