Accession Number : AD0614100

Title :   AN INTERPLANETARY DIFFUSION MODEL FOR THE TIME BEHAVIOR OF INTENSITY IN A SOLAR COSMIC RAY EVENT,

Corporate Author : IOWA STATE UNIV IOWA CITY

Personal Author(s) : Krimigis,S. M.

Report Date : 01 APR 1965

Pagination or Media Count : 63

Abstract : It is found possible to give a coherent interpretation of the time history of the intensity of several solar cosmic ray events in terms of a unified interplanetary diffusion model which assumes that the diffusion coeffieient D = M r to the B power, where r is the heliocentric radial distance and M and B are parameters, which may be dependent on particle energy E. The model is particularly successful in accounting for the decay phases. For the September 28, 1961 event M varies as E to the 0.33 power and, assuming spherical geometry, B is equal to one for 55 < E < 500 MeV and decreases rapidly at lower energies. At r = 1 A.U. the mean free path lambda is about 0.081 A.U. for E = 200 MeV and 0.15 for E = 23 MeV. The energy dependences of B and lambda suggest 0.006 A.U. as the order of magnitude of the scale size of irregularities in the interplanetary magnetic field. The source spectrum is inferred. The possibility of non-spherical geometry of diffusion is considered, as is the implication of the results with respect to the solar modulation of galactic cosmic radiation. (Author)

Descriptors :   (*COSMIC RAYS, DIFFUSION), (*SOLAR RADIATION, COSMIC RAYS), MATHEMATICAL MODELS, MAGNETIC FIELDS, PLANETS, PROTONS, PARTICLE TRAJECTORIES, SCATTERING, NUMERICAL METHODS AND PROCEDURES, FOURIER ANALYSIS

Distribution Statement : APPROVED FOR PUBLIC RELEASE