On the Interplanetary CosmicRay Scintillations
Abstract
The equation for the twoparticles cosmicray distribution function is derived by means of the Boltzmann kinetic equation averaging. This equation is valid for arbitrary ratio of regular and random parts of the magnetic field. For small energy particles the guidingcenter approximation is used. On the basis of the derived equation the dependence between power spectra of cosmicray intensity and random magnetic field is obtained. If power spectra are degree functions for high energy particles (≈ 10 GeV nucleon^{1}), then the spectral exponent υ of magnetic field lies between ϱ and ϱ2, where ϱ is the spectral exponent of cosmicray power spectra. The experimental data concerning moderate energy particles are in accordance with υ=ϱ, which demonstrates that the magnetic fluctuations are isotropic or cosmicray space gradient is small near the Earth orbit.
 Publication:

Astrophysics and Space Science
 Pub Date:
 May 1977
 DOI:
 10.1007/BF00648115
 Bibcode:
 1977Ap&SS..48..267T
 Keywords:

 Cosmic Rays;
 Distribution Functions;
 Interplanetary Medium;
 Radiation Distribution;
 Lines Of Force;
 Magnetic Variations;
 Power Spectra;
 Radiant Flux Density;
 Space Radiation