Abstract
Drifts have long been known to play a significant role in the transport and modulation of galactic cosmic rays (GCRs), occurring due to gradients in, as well as the curvature of, the heliospheric magnetic field (HMF). GCRs also drift along the wavy current sheet, a structure separating regions of opposite HMF polarity. Furthermore, the influence of drift effects is solar cycle dependent, as can, for example, be seen in the 22-year cycle observed in neutron monitor observations, corresponding to the 22-year HMF polarity cycle. As such, over the previous decades several techniques have been proposed to incorporate these effects into numerical cosmic ray modulation models. The present study compares the effects of employing these techniques, using a 3D, stochastic, ab initio GCR modulation model with a simulated solar cycle dependence. It is found that, for solar minimum conditions, all methods considered yield similar GCR intensities, but that the choice of method becomes significant when heliospheric conditions approaching solar maximum are to be modelled.
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