Numerical descriptions of cosmic-ray transport

Details Numerical descriptions of cosmic-ray transport Numerical descriptions of cosmic-ray transport

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4..396e&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 4 p 396-379 (SEE N85-34729 23-92)

Computer Science

Cosmic Rays, Fokker-Planck Equation, Magnetic Fields, Particle Diffusion, Radiation Transport, Steady State, Eigenvectors, Finite Difference Theory, Milne Method, Monte Carlo Method, Pitch (Inclination)

Scientific paper

The behavior of energetic particles in the solar system is described by a well known Fokker-Planck equation. Although analytic methods yield insight into the nature of its solutions, especially in the diffusion regime, calculations that go beyond diffusion are very complicated. The reliability of these calculations is of concern, because numerical methods are notorious for their errors and artifacts. The well known Milne problem of classical transport theory was analyzed with the aid of three different numerical methods. These are: (1) The method of eigenfunctions in which the distribution function is approximated by a sum of eigenfunctions of the scattering operator, (2) Numerical solutions of a finite difference aquation; and (3) Direct simulation of the scattering and streaming of individual particles with the aid of Monte Carlo methods.

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