Computer Science – Numerical Analysis
Scientific paper
Aug 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....8.3215b&link_type=abstract
Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int
Computer Science
Numerical Analysis
8
Solar Corona, Shock Waves, Particle Diffusive Shock Acceleration, Solar Cosmic Rays, Shock Fronts, Solar Wind, Solar Terrestrial Interactions, Energy Spectra, Numerical Analysis, Time Dependence, Alfven Waves, Particle Emission
Scientific paper
Energetic particle (ion) acceleration by shocks during their propagation through the solar corona is studied. Diffusive transport equation is solved numerically within the range of heliocentric distance up to 3 solar radius, where the efficient particle acceleration takes place. The values of corona parameters are taken from the observations. Due to high level of background Alfv´enic turbulence and shock speed values the spectrum of accelerated particles is quickly formed during the initial period of shock propagation up to maximum energy of the order of 1 GeV. On later stages acceleration process becomes inefficient due to the decrease of Alfv´enic Mach number and previously produced particles start to run away from the shock due to their progressively increasing mobility. These particles are presumably observed in the interplanetary space as so called solar energetic particle (SEP) event. Performed calculations demonstrate that the main characteristics of accelerated particles ( their upper energy, spectral shape, energy content) are consistent with what is required to produce the observed SEP events.
Berezhko Evgeny G.
Petukhov S. I.
Taneev S. N.
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