Motion of solar cosmic rays in the coronal magnetic field

Details Motion of solar cosmic rays in the coronal magnetic field Motion of solar cosmic rays in the coronal magnetic field

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979soph...62..153m&link_type=abstract

Solar Physics, vol. 62, May 1979, p. 153-177. NSF-supported research.

Physics

9

Particle Motion, Particle Trajectories, Solar Corona, Solar Cosmic Rays, Solar Magnetic Field, Three Dimensional Motion, Diffusion Coefficient, Drift Rate, Graphs (Charts), Life (Durability), Particle Acceleration, Proton Scattering, Solar Flares, Solar Physics, Solar Terrestrial Interactions, Synoptic Measurement

Scientific paper

Three-dimensional trajectories of solar cosmic rays as they propagate through the corona are calculated by assuming a strictly static large-scale coronal magnetic field. Empirical drift and diffusion rates over a wide range of energies are summarized, and the trajectory code is described with special reference to magnetic-field evaluation. Results obtained both with and without scattering centers are presented and compared with observational data. It is proposed that if a flare occurs far from a sun-earth field line, particle propagation due to magnetic-bottle expansion must be supplemented by a second component of propagation due to diffusion.

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