  After the disappearance of lower energy heliospheric particles at Voyager 1
starting on August 25th, 2012, spectra of H, He and C/O nuclei were revealed
that resembled those to be expected for galactic cosmic rays. These spectra had
intensity peaks in the range of 30-60 MeV, decreasing at both lower energies
down to a few MeV and at higher energies up to several hundred MeV. We have
modeled the propagation of these particles in the galaxy using an updated Leaky
Box Diffusion model which determines the spectra of these components from ~2
MeV to >200 GeV. The key parameters used in the model are a galactic input
spectrum ~P^-2.24, the same for all components and independent of rigidity, and
a 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 the
high energy H and He data from ~10-200 GeV/nuc from the PAMELA and BESS
experiments. The new Voyager spectra for all three nuclei are thus consistent
with rigidity spectra ~P^-2.24 from the lowest energies to at least 100 GeV.
Deviations from this spectrum can reasonably be attributed to propagation
effects. Some deviations between the calculated and newly observed spectra are
noted, however, below ~30 MeV/nuc, particularly for C/O nuclei, that could be
significant regarding the propagation and sources of these particles.
