Modeling the behavior of the cosmic ray density in magnetic clouds

Our study focuses on the behavior of the density of cosmic ray particles at 10 GV rigidity in a magnetic cloud at Earth. It is shown that it can be mostly described by a simple parabolic dependence over distance from the centre of the cloud, when measured in gyroradii. The majority of magnetic clouds modulate cosmic rays, decreasing their density. However, there is a group of events (about 1/5 part of the total sample) during which the cosmic ray density increases within the magnetic cloud. The factors that contribute to the model description are considered, and estimates of their influence are carried out and discussed.