The energetic charged particle propagation in the heliospheric magnetic fields is considered on the base of cosmic ray transport equation. The transport equation solution is reached in the approximation of small anisotropy value of particle angular distribution. The galactic cosmic ray energetic distribution at the heliopause is used as a transport equation boundary condition. The cosmic ray energy spectrum in the local interstellar medium is supposed to be known due to the results of prominent space missions (Pioneer, Voyager, PAMELA, AMS-02 etc.). The density of cosmic ray streaming is calculated during periods of various solar magnetic polarities. It is shown that the galactic cosmic ray intensity is minimal near the helioequator during periods of positive magnetic polarity. Under negative interplanetary magnetic field polarity the cosmic ray intensity decreases if the heliolatitude increases.