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Using Leaky Box Model propagation calculations for H nuclei and a Monte Carlodiffusion propagation model for electrons, starting from specific sourcespectra, we have matched the observed LIS spectra of these cosmic rays measuredby Voyager at lower energies and AMS-2 at higher energies, a range from ~10 MeVto ~1 TeV. The source spectra required are very similar rigidity spectra. Below~6-10 GV the source spectra for both particles are ~P-2.25 and above 10 GV thespectra are ~P-2.36-2.40. This break in the source spectral index is not seenfor He and C nuclei in a match of Voyager and AMS-2 intensities both of whichhave source rigidity spectra with an index ~-2.24 throughout the entire rangeof measured energies from ~10 MeV//nuc to ~1 TeV/nuc. The absolute sourceintensities of electrons and H nuclei are derived and the source ratio ofaccelerated electrons to H nuclei is between 2-5%. The total number ofaccelerated electrons is much greater than that for protons, however, becausethe accelerated electron spectrum extends down to ~1-2 MV rigidity whereas theH nuclei spectrum cannot be observed below ~50-100 MV because of ionizationenergy loss. Most of these low energy electrons escape from the galaxy formingan intergalactic background.

A Comparison of the Galactic Cosmic Ray Electron and Proton Intensities  From 1 MeV/nuc to 1 TeV/nuc Using Voyager and Higher Energy Magnetic  Spectrometer Measurements Are There Differences in the Source Spectra of  These Particles?