Propagation of Galactic Cosmic Rays in the Heliosphere during Minimum Solar Activity Periods

Abstract

Based on the cosmic ray transport equation, the propagation of charged high-energy particles in heliospheric magnetic fields is considered. The transport equation solution is found in the approximation of low anisotropy in the angular distribution of particles. The energy distribution of galactic cosmic rays at a heliopause is used as a boundary condition. The energy spectrum of cosmic rays in a local interstellar space is considered to be known due to the outstanding results of space missions (Pioneer, Voyager, PAMELA, AMS-02, etc.). The flux density of cosmic rays is calculated in the periods of different solar magnetic polarity. It is shown that the intensity of galactic cosmic rays in positive magnetic polarity periods is maximum near the helioequator. In the periods when the interplanetary magnetic field has a negative polarity, the intensity of cosmic rays decreases with increasing heliolatitude.