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After the disappearance of lower energy heliospheric particles at Voyager 1starting on August 25th, 2012, spectra of H, He and C/O nuclei were revealedthat resembled those to be expected for galactic cosmic rays. These spectra hadintensity peaks in the range of 30-60 MeV, decreasing at both lower energiesdown to a few MeV and at higher energies up to several hundred MeV. We havemodeled the propagation of these particles in the galaxy using an updated LeakyBox Diffusion model which determines the spectra of these components from ~2MeV to >200 GeV. The key parameters used in the model are a galactic inputspectrum ~P^-2.24, the same for all components and independent of rigidity, anda diffusion coefficient that is ~P^0.5 above a lower rigidity and increases~beta^-1.0 below a lower rigidity ~0.56 GV. These same parameters also fit thehigh energy H and He data from ~10-200 GeV/nuc from the PAMELA and BESSexperiments. The new Voyager spectra for all three nuclei are thus consistentwith rigidity spectra ~P^-2.24 from the lowest energies to at least 100 GeV.Deviations from this spectrum can reasonably be attributed to propagationeffects. Some deviations between the calculated and newly observed spectra arenoted, however, below ~30 MeV/nuc, particularly for C/O nuclei, that could besignificant regarding the propagation and sources of these particles.

A Comparison of the Galactic Cosmic Ray H, He and C/O Nuclei Spectra  Measured Between ~5 and 500 MeV/nuc Beyond 122 AU at Voyager 1 with the  Predictions of a Diffusion Model for Propagation in the Galaxy