Shock Acceleration of Solar Cosmic Rays

Details Shock Acceleration of Solar Cosmic Rays Shock Acceleration of Solar Cosmic Rays

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003astl...29..530b&link_type=abstract

Astronomy Letters, vol. 29, p. 530-542 (2003)

Computer Science

Numerical Analysis

11

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

We investigated the acceleration of solar cosmic rays (SCRs) by the shock waves produced by coronal mass ejections. We performed detailed numerical calculations of the SCR spectra produced during the shock propagation in the solar corona in terms of a model based on the diffusive transport equation using a realistic set of physical parameters for the corona. The resulting SCR energy spectrum N(E) E^{-gamma}exp[-(E/E_max)alpha] is shown to include a power-law portion with an index gamma 2 that ends with an exponential tail with alpha = 2.5 - beta, where beta is the spectral index of the background Alfven turbulence. The maximum SCR energy lies within the range E_max=1-300 MeV, depending on the shock velocity. Because of the steep spectrum of the SCRs, their backreaction on the shock structure is negligible. The decrease in the Alfven Mach number of the shock due to the increase in the Alfven velocity with heliocentric distance r causes the efficient SCR acceleration to terminate when the shock reaches a distance of r = 2-3 R_solar. Since the diffusive SCR propagation in this case is faster than the shock expansion, SCR particles intensively escape from the shock vicinity. A comparison of the calculated SCR fluxes expected near the Earth's orbit with available experimental data indicates that the theory satisfactorily explains all of the main observed features.

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