Numerical analysis of the azimuthal transport of solar particles

Details Numerical analysis of the azimuthal transport of solar particles Numerical analysis of the azimuthal transport of solar particles

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987rmxaa..14..693p&link_type=abstract

(IAU, Reunion Regional Latinoamericana de Astronomia, 5th, Merida, Mexico, Oct. 6-10, 1986) Revista Mexicana de Astronomia y Ast

Computer Science

Numerical Analysis

Numerical Analysis, Particle Motion, Solar Corona, Solar Corpuscular Radiation, Solar Flares, Solar Magnetic Field, Energy Spectra, Interplanetary Magnetic Fields, Magnetic Field Configurations, Magnetic Flux, Solar Atmosphere, Solar Protons

Scientific paper

An account is given of magnetic field structure details within the framework of analytical methods previously used by Perez-Peraza (1986) to describe global features of global azimuth transport phenomena involving particles generated in solar flares. A numerical solution is furnished for the model developed; particle energy spectra are derived at the level of the coronal magnetic field's roots for two specific proton events. Characteristics of the large-scale coronal magnetic field topology can be inferred by comparing these spectra with those derived from the interplanetary demodulation of solar proton data at the level of the earth.

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