A numerical model for studying the influence of the large-scale shock topology on the associated low-energy (less than 2 MeV) particle event upstream of the shock is presented. It includes particle injection at the solar corona, 2D MHD simulation of the propagation of the shock, modeling of particle propagation through the interplanetary medium, and particle injection at the shock. The MHD simulation determines the time when the shock intersects the interplanetry magnetic field line which connects with the spacecraft, the evolution of this connection point over the shock front, and its plasma characteristics as it propagates out into the heliosphere. The parameters which characterize particle propagation and the rate of particle injection at the shock front are determined. It is therefore possible to infer the history of the development of the particle event and to analyze the possible relations with the parameters at the point of the shock that is, at each moment, magnetically connected with the spacecraft.
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Heras et al. (1992) studied this question.