The expected cosmic ray density and stream distributions at the heliolatitudinal asymmetry of solar wind
Abstract
The results of the spatial distribution of cosmic ray density, gradients, and anisotropy obtained on the basis of the numerical solution of the anisotropic diffusion equation with an account of solar wind velocity change depending on the latitudinal angle theta of the form U=u_{oe}^{alpha} theta and the diffusion coefficient depending on the spatial coordinates and the particle rigidity are presented. It is shown that the increase of the solar wind velocity and the diffusion coefficient with heliolatitude leads to gradient distributions that are in accord with experimental data observed in space. The results of the energetic spectrum of 11 and 22year cosmic ray variations obtained with an account of direction of the general magnetic field of the Sun are presented are given.
 Publication:

19th International Cosmic Ray Conference (ICRC19), Volume 4
 Pub Date:
 August 1985
 Bibcode:
 1985ICRC....4..465A
 Keywords:

 Anisotropy;
 Asymmetry;
 Coronal Holes;
 Diffusion Coefficient;
 Galactic Cosmic Rays;
 Gradients;
 Particle Density (Concentration);
 Rigidity;
 Solar Cycles;
 Solar Magnetic Field;
 Solar Wind Velocity;
 Spatial Distribution;
 Cosmic Ray Showers;
 Interplanetary Space;
 Pioneer 10 Space Probe;
 Pioneer 11 Space Probe;
 Radio Astronomy;
 Space Radiation