Based on the lighting waveform and spectra observed by the Galileo Atmospheric Probe, we present a discharge, radiation, and propagation model of the Jovian lighting that explains the absence of detectable HF spherics along with the measurement of ELF whistler emissions by the Voyager radio and plasma wave instruments. We find that although there is signal attenuation in the ionosphere, the controlling factor in determining lighting detectability at Jupiter is the intrinsically slow nature of the lighting discharge itself. The proposed discharge model is not unique, but matches the observed spectrum which spans several frequency decades and provides a basis for comparing lighting discharge models for other planets. ¿ 1999 American Geophysical Union