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

Space Physics