Data from the Energetic Particle Detector on Galileo have been used to investigate whether the radiation belt population can act as a direct energy reservoir for Jovian auroral emissions. Energetic (E>42 keV) ion distributions in the middle magnetosphere (9<RJ<26) yield peak precipitation energy fluxes comparable to a few ergs-cm-2-s-1, which are too weak to produce significant auroral emissivity. Detailed analysis of energetic electrons (15--884 keV) indicates the presence of an enhanced population near the loss cone that may provide precipitation energy flux above 10 ergs-cm-2-s-1 over an extended region (10≤RJ≤25) of the middle magnetosphere. The available precipitation electron energy flux decreases at higher radial distance, falling to values below 1 erg-cm-2-s-1 outside 30RJ. Additional acceleration mechanisms such as field-aligned currents are required to account for observed auroral intensities at higher L. The precipitation flux values presented here have been calculated under the assumption of strong pitch-angle scattering due to wave-particle interactions in the essentially collisionless middle magnetosphere. Plasma waves with relatively modest amplitude (Bw≥25 pT or Ew≥5 mV/m) are sufficient to induce strong diffusion scattering outside 10 RJ. Such scattering can account for energy deposition over a broad latitude range (Δ&lgr;≥5¿) associated with the diffuse Jovian aurora. ¿ 2001 American Geophysical Union