Abstract
The characteristics of the Jovian radio emission are described. The emission is in the form of intermittent bursts in the frequency range 10 to 35 Mc, with a maximum at 18 Mc, and it appears to come from a localized source with directional properties on Jupiter. The evidence indicates that the Jovian broadcasts are initiated by solar particles. lt is suggested that the emission is a decameter emission from electrons making spin-flip transitions in the perturbed magnetic field of Jupiter. Impinging clouds of solar particles could trigger the oscillating magnetic perturbations which would then cause the electrons to make the transitions. The Jovian magnetic field is calculated to be 6.4 gauss at the altitude where the emission occurs. From the observed power of the emission, the rate of electron spinflips is calculated to be ~10/sup 5//sec. The cause of the emission variation with the phase of the Jovian day is discussed.
Published Version
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