DRIFT MODELS AND POLAR FIELD FOR COSMIC RAYS PROPAGATION IN THE HELIOSPHERE

We developed a two dimensional (2D) Stochastic Montecarlo code for the Cosmic Rays propagation in the Heliosphere. We used the most recent observations in order to model drift, polar field geometry and Solar Wind latitudinal dependence and to reproduce the measured fluxes. We tested 3 different drift models and compared results with data of AMS-01, IMAX, CAPRICE and BESS 2002, finding the best set of parameters for different periods of solar activity