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Data of super neutron monitors, Bx, By, Bz components of the interplanetary magnetic field (IMF) a have been used to study a relation of the long-period variations of the galactic cosmic ray (GCR) intensity with IMF turbulence for the period of 1968-2014. We find that the changes of the rigidity spectrum exponent γ of the GCR intensity variations and the exponents vy, νz, νx of the power spectral density (PSD) of the By, Bz, Bx components show a radical alternation of the large–scale structure of the IMF turbulence in period 1968-2014. We also study the properties of the probability distribution function (PDF) of the Bx, By, Bz components and their differences δBi=Bi(t+τ)-Bi(t) (i=x, y, z) of the IMF, over the varying time scales τ=1,2,3,4,5 days. We find that for the time scales τ  4 days the skewness and kurtosis of the IMF turbulence almost equal zero. So, at first approximation, one can state that the PDFs are almost Gaussian and anisotropy and inhomogeneous of the IMF turbulence can be ignored in large vicinity of space (10 cm). However, for smaller vicinity of space (<10 cm ) the turbulence of the solar wind plasma can be an anisotropic. As a result, for large part of space one can state that IMF turbulence could be fully described by the parameters of PSD = P ∙ f (P-power and ν– exponent) and employ to calculation of transport coefficients of GCR in heliosphere.

proceedings of the 34th international cosmic ray conference — pos(icrc2015)

FEATURES OF LONG PERIOD VARIATIONS OF GALACTIC COSMIC RAY INTENSITY IN RELATIONS WITH THE TURBULENCE OF THE INTERPLANETARY MAGNETIC FIELD in 1968 - 2014