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Observationally, it is difficult to establish at what rigidity the modulationof galactic cosmic rays (CRs) actually begins in the heliosphere. It should bepossible to do if the relevant local interstellar CR spectra were known andreliable measurements were made between 10 GV and about 200 GV, inside andoutside the heliosphere. Numerical models for solar modulation studies arebased on simply assuming that CR modulation begins at a given spatial boundaryand at rigidities between 30 to 50 GV, usually handled as an initial condition.The Stochastic Differential Equations approach to numerical modelling presentsthe opportunity to determine the level of modulation from high to lowrigidities because an initial condition at a prescribed high rigidity is notrequired. We present the results of such an approach and show the percentagemodulation of CR protons as a function of kinetic energy between 100 MeV and250 GeV.

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