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The cosmic ray electrons measured by Voyager 1 between 3-70 MeV beyond theheliopause have intensities several hundred times those measured at the Earthby PAMELA at nearly the same energies. This paper compares this new V1 datawith data from the earth-orbiting PAMELA experiment up to energies greater than10 GeV where solar modulation effects are negligible. In this energy regime weassume the main parameters governing electron propagation are diffusion andenergy loss and we use a Monte Carlo program to describe this propagation inthe galaxy. To reproduce the new Voyager electron spectrum, which is E-1.3,together with that measured by PAMELA which is E-3.20 above 10 GeV, we requirea diffusion coefficient which is P 0.45 at energies above 0.5 GeV changing to aP-1.00 dependence at lower rigidities. The entire electron spectrum observed atboth V1 and PAMELA from 3 MeV to 30 GeV can then be described by a simplesource spectrum, dj/dP P-2.25, with a spectral exponent that is independent ofrigidity. The change in exponent of the measured electron spectrum from -1.3 atlow energies to 3.2 at the highest energies can be explained by galacticpropagation effects related to the changing dependence of the diffusioncoefficient below 0.5 GeV, and the increasing importance above 0.5 GV of energyloss from synchrotron and inverse Compton radiation, which are both E2, andwhich are responsible for most of the changing spectral exponent above 1.0 GV.  As a result of the P-1.00 dependence of the diffusion coefficient below 0.5GV that is required to fit the V1 electron spectrum, there is a rapid flow ofthese low energy electrons out of the galaxy. These electrons in local IG spaceare unobservable to us at any wave length and therefore form a dark energycomponent which is 100 times the electrons rest energy.

The Galactic Cosmic Ray Electron Spectrum from 3 to 70 MeV Measured by  Voyager 1 Beyond the Heliopause, What This Tells Us About the Propagation of  Electrons and Nuclei In and Out of the Galaxy at Low Energies