Interplanetary cosmic-ray scintillations
Toptygin, I N; Vasiliev, V N [Kalininskij Sel'skokhozyajstvennyj Inst. (USSR)]
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; COSMIC RADIATION; DISTRIBUTION FUNCTIONS; INTERPLANETARY MAGNETIC FIELDS; SCINTILLATIONS; INTERPLANETARY SPACE; FLUX DENSITY; BOLTZMANN EQUATION; CORRELATION FUNCTIONS; ELECTRIC FIELDS; FLUCTUATIONS; GREEN FUNCTION; ITERATIVE METHODS; KINETIC EQUATIONS; POWER; SOLAR WIND; SPECTRA; DIFFERENTIAL EQUATIONS; EQUATIONS; FUNCTIONS; IONIZING RADIATIONS; MAGNETIC FIELDS; RADIATIONS; SOLAR ACTIVITY; SPACE; VARIATIONS; 640105* - Astrophysics & Cosmology- Galaxies; 640101 - Astrophysics & Cosmology- Cosmic Radiation
The equation for the two-particles cosmic-ray 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 guiding-center approximation is used. On the basis of the derived equation the dependence between power spectra of cosmic-ray intensity and random magnetic field is obtained. If power spectra are degree functions for high energy particles (approximately 10 GeV nucleon/sup -1/), then the spectral exponent ..gamma.. of magnetic field lies between rho and rho-2, where rho is the spectral exponent of cosmic-ray power spectra. The experimental data concerning moderate energy particles are in accordance with ..gamma..=rho, which demonstrates that the magnetic fluctuations are isotropic or cosmic-ray space gradient is small near the Earth orbit.
Netherlands
1977-05-01
English
Journal Article
Journal Name: Astrophys. Space Sci.; (Netherlands); Journal Volume: 48:2
Medium: X; Size: Pages: 267-281
https://doi.org/10.1007/BF00648115
Journal ID: CODEN: APSSB
INIS; AIX-08-342097; EDB-78-040192
2010-12-29
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