Physics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..139..189v&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 139, no. 1, May 1992, p. 189-199. Research supported by SERC.
Physics
12
Cosmic Rays, Diffusion Coefficient, Heliosphere, Interplanetary Magnetic Fields, Particle Diffusion, Particle Trajectories, Power Spectra, Protons, Voyager 2 Spacecraft
Scientific paper
A model of the cross-field diffusion of the interplanetary magnetic field (IMF) is developed which incorporates Voyager 2 data from 14.8 AU. A simulation technique by Moussas et al. (1982) is adapted for perpendicular diffusion, and the data from the Voyager are employed to calculate the perpendicular diffusion coefficients numerically. The simulation developed measures the small-scale random gradient and curvature drifts as well as cross-field resonance scattering, although field-line wandering is not incorporated. The perpendicular diffusion coefficient is found to be (2.8 + or - 0.9) x 10 exp 21 sq cm/s, a value which is substantially greater than the result previously obtained for 5 AU. The results suggest that the corresponding value of beta is approximately equal to 0.8-1.1 for an assumed power-law radial dependence. Observational data for the cosmic-ray radial gradient are shown to support the present analytical values.
Moussas Xenophon
Quenby John J.
Valdés-Galicia Francisco J.
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