Keywords
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
Solar Physics
Solar Corona:Particle Propagation
Solar Corona:Protons
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
Solar Physics
Solar Corona:Particle Propagation
Solar Corona:Protons
How to Cite
Numerical analysis of the azimuthal transport of solar particles. (1987). Revista Mexicana De Astronomía Y Astrofísica, 14(1), 693-699. https://astronomia.unam.mx/journals/rmxaa/article/view/1987rmxaa..14..693p
Abstract
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.Similar Articles
- Martinell J., Perez-Peraza J., Coronal transport of solar flare particles , Revista Mexicana de Astronomía y Astrofísica: Vol. 6 No. 1 (1981)
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