Abstract
The longitudinal distribution of the intensity of the solar cosmic ray (SCR) flux in the heliosphere during different stages of powerful proton events in 2012 is considered, based on the data from the SOHO and STEREO-A and -B spacecraft separated by ∼120° at 1 AU. The SCR distribution during an event’s initial stage corresponds to the belief that the role of the magnetic connection between a source and an observer (the arrival of protons from west, central, and east parent flares) is important. The convection of SCRs changes the relationship between the intensities observed by different spacecraft, when the structures containing SCRs reach any spacecraft as a result of a radial or co-rotational solar wind motion. The SCR intensities during the late prolonged decay phase are approximately equal (the reservoir effect) at points separated by 120° (STEREO A/B and/or SOHO). The reservoir effect is observed not only behind a shock front but also over a much wider region, indicating that the role of perpendicular diffusion in the SCR propagation is crucial.
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