Physics
Scientific paper
Dec 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979soph...64..391s&link_type=abstract
Solar Physics, vol. 64, Dec. 1979, p. 391-401.
Physics
1
Diffusion Coefficient, Energetic Particles, Particle Diffusion, Plasma-Particle Interactions, Solar Cosmic Rays, Solar Wind, Mean Free Path, Solar Flares, Solar Magnetic Field
Scientific paper
Theoretical considerations lead to a solar cosmic ray diffusion coefficient which varies with heliolongitude in a stream-structured solar wind. By solving numerically the time dependent convection-diffusion equation for the particle transport, the effect of the azimuthal variation of the diffusion coefficient is investigated on intensity-time profiles as seen by a stationary observer. Depending on the position of the observer relative to the solar wind stream at the time of flare occurrence, completely different intensity-time profiles will be observed. When the spacecraft is at the time of the flare occurrence right at the leading edge of a solar wind stream, the large mean free path leads to rapid steepening of the initial phase of the intensity profile. The longitudinally decreasing mean free path of about 1 day in front of the leading edge will lead to intensity-time profiles similar to long-time injection events if the event occurs before the stationary observer enters the flux tubes with the decreasing diffusion coefficient.
Morfill Gregor
Richter Arne K.
Scholer Manfred
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