Anisotropic diffusion of galactic cosmic rays with accounting for the real distribution of solar activity

By the net method the anisotropic diffusion equation is solved which describes galactic cosmic ray propagation in a stationary regime to find out the density distribution, radial and transverse gradients of galactic cosmic rays. It is supposed that the transport range for particle scattering by magnetic inhomogeneities of the solar wind is controlled by intensity of the green coronal line (GCL)Λ=5303 A. On the base of anisotropic diffusion equation solution the spectrum of the 11 year cosmic rays variation is determined. The analysis of the results obtained shows that using the GCL intensity as solar activity parameter the modulation depth and radial gradient of cosmic rays at the r<3-5 a.e. distance are considerably more than in the case when the sunspot area is such a parameter. At more distances the modulation depth and gradient changes are of a smooth character. Abrupt changes of characteristics given are neither observed when GCL is a parameter and when data on sunspot areas are used