Transport of a few-MEV jovian and galactic electrons at solar maximum

Abstract

The heliospheric modulation of galactic and jovian electrons is studied using a three-dimensional, steady-state model based on Parker's transport equation including the jovian source. The model is developed to study both jovian and galactic electrons. It is illustrated how the electron intensity-time profile along the Ulysses trajectory is effected as compared to the 3–10 MeV electron flux observed from its launch until the recent solar maximum conditions by varying. The relative contributions of the jovian and galactic electrons to the total electron intensity is also shown along the Ulysses trajectory. For this changes in the solar wind speed, the jovian source strenght and the diffusion tensor are made. To explain these observations we find that the enhancement of the perpendicular diffusion coefficient toward the heliospheric poles must be reduced with increasing solar activity.