Description of galactic cosmic ray intensity in the last three solar activity minima

Abstract

Using a numerical solution to the transport equation for galactic cosmic rays, the behavior of the intensity is described within a simple heliosphere model for the last three solar activity minima. The model differs from the ones we used earlier in the area of drift velocities, and in allowing for the difference between the characteristics of the heliospheric magnetic field inside and outside the sector zone. The results from calculations are compared with measurement data obtained for the intensity of galactic cosmic rays according to regular balloon monitoring in the Earth’s atmosphere.