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The results of numerical integrations of the rates and emissivities of the photo, pair, and plasma neutrino emission mechanisms in the Weinberg-Salam theory of the weak interaction are presented. We consider the range of densities 10 gm cm-s 5 p < lOI gm cm-s and the temperature range 10sK 5 T 5 10°K. We present fitting formulae, similar to those provided by Beaudet, Petrosian, and Salpeter (1967), which reproduce our numerical result for the total emissivity to within 20% in the temperature range 10s2K 5 T 5 10°K.

The energy spectra and pitch angle distributions of energetic protons injected into the inner Saturnian magnetosphere by the cosmic ray albedo neutron decay (CRAND) process have been calculated using the nucleon transport code HETC. These calculations predict spectra and pitch angle distributions consonant with the Pioneer and Voyager observations for proton energies above ∼50 MeV assuming that the ring particles are ice, not rock, and that the mean mass seen by the cosmic rays is several tens to a few hundred grams per square centimeter.

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