Three distinct bands of whistler mode emissions were detected by the Voyager 1 and Voyager 2 plasma wave instruments during the encounter with Jupiter. The broadband whistler mode hiss below 1 kHz and two narrowbanded, high-frequency emissions near 10 kHz were identified as whistler mode chorus and half electron cyclotron emission. In the present analysis the entire electron velocity space distribution is modeled by a superposition of three anisotropic components, two kappa distributions of different spectral index, and a drifting Maxwellian distribution. Applying a linear instability analysis on this specific distribution and providing the basic plasma parameters from spacecraft observations yields a highly accurate picture of the structure of the observed discrete Jovian whistler emission spectrum. It is concluded that the generation of the hiss structure can be interpreted to be a consequence of resonating suprathermal non-Maxwellian electrons, whereas the chorus is generated by a nearly bi-Maxwellian population. The half electron cyclotron emission can be associated with the interaction of a drifting, anisotropic component of keV electrons. The analysis of the main emission bands of a specific full spectrum can serve as representative pattern for the interpretation of various whistler mode events in planetary magnetospheres. ¿ 2000 American Geophysical Union