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In this paper we fit the observed galactic cosmic ray electron spectrum froma few MeV to 1 TeV. New data from Voyager from 5-60 MeV beyond the heliopauseis used along with high energy data from the PAMELA, FERMI and AMS-2instruments in Earth orbit. Using a Monte Carlo diffusion model for galacticpropagation we obtain a source rigidity spectrum with a spectral index =-2.25independent of energy below 10 GeV, possibly steepening above 10 GeV to 2.40 atthe highest energies. This spectrum will fit the electron data over 5 orders ofmagnitude to within + 10% at both low and high energies. This steepening of theelectron source spectrum could be an important feature of the accelerationprocess, e.g., synchrotron loss during acceleration could steepen the sourcespectrum. This fit requires only a single break in the rigidity dependence ofthe diffusion coefficient by ~1.0 power in the exponent at about 1.0 GV. Thecalculations also predict the distribution of electrons perpendicular to thegalactic disk. The galaxy does act as a calorimeter for electrons in the energyrange 0.1-10 GeV where ~80% of the electrons are trapped. At higher energiesthe electrons escape the galactic disk rapidly. At energies ~1 TEV theelectrons loose most of their energy by synchrotron and inverse Comptonemission within < 0.5 Kpc of their origin near the galactic equator. Atenergies < 0.1 GeV, because of the increase in the diffusion coefficient below~1 GV, and the absence of other significant loss processes, the electronsescape and form a difficult to detect, but important galactic halo population.

A Galactic Cosmic Ray Electron Spectrum from 2 MeV to 2 TeV That Fits  Voyager 5-60 MeV Data at Low Energies and PAMELA and AMS-2 Data at 10 GeV  Using an Electron Source Spectrum E^-2.25 A Calculation Using a Monte Carlo  Diffusion Model