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Diffusive shock acceleration (DSA), as an acceleration process for Galacticelectrons at the solar wind termination shock (TS), is investigated with acomprehensive numerical model which incorporates shock-acceleration, particledrifts and other major modulation processes in the heliosphere. It is knownfrom our previous work that the efficiency of DSA depends on the shape ofelectron spectra incident on the TS, which in turn depends on the spectralshape of the very local interstellar spectrum. Modulation processes alsoinfluence the efficiency of DSA. We find that TS accelerated electrons can makecontributions throughout the heliosphere to intensity levels, especially atlower energies. An interesting result is that increases caused by DSA at the TSare comparable in magnitude to electron intensity enhancements observed byVoyager 1 ahead of the TS crossing. These intensity increases are large enoughto account for observed intensity peaks, and thus supports the view that DSA isinvolved in their production. Additionally, the energy spectra observed byVoyager 1 throughout the heliosheath are reproduced satisfactorily, as well asthe PAMELA spectrum at Earth at higher energies. We also find that an increasein the rigidity dependence of the diffusion coefficients for these low-energyelectrons seems required to reproduce the spectral shape of observed modulatedspectra in the heliosheath at kinetic energy E < ~ 4 MeV. This is differentfrom intermediate energies where rigidity independent diffusion explainsobservations satisfactory.

Acceleration of galactic electrons at the solar wind termination shock and Voyager 1 observations