A three-dimensional, steady state, numerical model was used to model the propagation of 7 MeV jovian and galactic electrons in the heliosphere. The computations are compared with 3--10 MeV Ulysses/KET electron observations which are still not well explained after ~1998. To explain these observations, coinciding with solar maximum conditions, it is shown that a reduction in the enhancement of perpendicular transport toward the poles is required compared to solar minimum. The decrease in this enhancement can be correlated to the disappearance of the fast solar wind and/or a heliospheric magnetic field with a meridional component at solar maximum. By assuming a substantial jovian contribution to the total low-energy electron intensity at high latitudes to explain the Ulysses/KET observations in these regions, important information on the magnitude of perpendicular transport in the polar direction and its time dependence can be deduced.