At what Rigidity does the Solar Modulation of Galactic Cosmic Rays begin?

Observationally, it is difficult to establish at what rigidity the modulation of galactic cosmic rays (CRs) actually begins in the heliosphere. It should be possible to do if the relevant local interstellar CR spectra were known and reliable measurements were made between 10 GV and about 200 GV, inside and outside the heliosphere. Numerical models for solar modulation studies are based on simply assuming that CR modulation begins at a given spatial boundary and at rigidities between 30 to 50 GV, usually handled as an initial condition. The Stochastic Differential Equations approach to numerical modelling presents the opportunity to determine the level of modulation from high to low rigidities because an initial condition at a prescribed high rigidity is not required. We present the results of such an approach and show the percentage modulation of CR protons as a function of kinetic energy between 100 MeV and 250 GeV.