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Shock acceleration of energetic particles in corotating interaction regions in the solar wind
Fisk, L. A.; Lee, M. A.
AA(New Hampshire, University, Durham, N.H.), AB(New Hampshire, University, Durham, N.H.)
Astrophysical Journal, Part 1, vol. 237, Apr. 15, 1980, p. 620-626. (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Energetic Particles, Particle Acceleration, Particle Interactions, Rotating Plasmas, Shock Waves, Solar Wind, Adiabatic Conditions, Diffusion Coefficient, Interplanetary Medium, Magnetic Flux, Magnetohydrodynamics, Mathematical Models, Shock Fronts, Stellar Models
Bibliographic Code:


A simple shock model for the acceleration of energetic particles in corotating interaction regions (CIRs) in the solar wind is presented. Particles are accelerated at the forward and reverse shocks which bound the CIR by being compressed between the shock fronts and magnetic irregularities upstream from the shocks, or by being compressed between upstream irregularities and those downstream from the shocks. Particles also suffer adiabatic deceleration in the expanding solar wind, an effect not included in previous shock models for acceleration in CIRs. The model is able to account for the observed exponential spectra at earth, the observed behavior of the spectra with radial distance, the observed radial gradients in the intensity, and the observed differences in the intensity and spectra at the forward and reverse shocks.

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Database: Astronomy
arXiv e-prints