  Utilizing new Voyager measurements at lower energies and higher energy
spacecraft measurements near the Earth, the interstellar spectra of primary
cosmic ray nuclei from H to Fe have now been determined from ~10 MeV/nuc to >
100 GeV/nuc. These measurements are compared with the predictions from a Leaky
Box propagation model. It is found that above ~50-100 MeV/nuc the spectra of
all the nuclei, H, He, C, O, Ne, Mg, Si and Fe are well connected between 100
MeV/nuc and 10 GeV/nuc and above by simple source rigidity spectra proportional
to P-2.28, with the exponent independent of rigidity and using a rigidity
dependent diffusion coefficient ~P0.50 above ~1.0 GV. This leads to intensities
and spectra ~P-2.78 at ~100 GeV/nuc and above, which are consistent with new
AMS-2 and PAMELA measurements of H, He and C to within + 10%.
  Below 50-100 MeV the spectra of these primary charges fall into two groups.
The spectra of primary nuclei with Z > 6 fall more rapidly at low energies than
those of H and He and more rapidly than would be expected from a pure diffusive
LBM, where energy loss by ionization is important at low energies. Increasing
the fraction of ionized hydrogen in the interstellar medium from 15% to 30%
does not satisfactorily explain the systematics of the intensity decreases of
the heavier primary nuclei at low energies. Other processes beyond those
assumed in a simple leaky box model, such as a lack of cosmic ray sources near
the Sun are being investigated as the source of this more rapid intensity
decrease of these nuclei.
  The spectra of H and He are very similar to each other but both contain more
low energy particles than would be expected from a correspondence with the
heavier nuclei spectra. We believe that this may indicate the presence of a
local (heliospheric) component of these nuclei in addition to the galactic
component.
