Abstract A simple shock model for the acceleration of energetic particles in corotating interaction regions (CIR) 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 CIR's. 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.
Shock acceleration of energetic particles in corotating interaction regions
Advances in Space Research ; 1 , 3 ; 93-96
1981-01-01
4 pages
Article (Journal)
Electronic Resource
English
Acceleration in energetic ions (1 MeV) in corotating interaction regions
Online Contents | 1998
|British Library Conference Proceedings | 1997
|Acceleration in energetic ions (asymptotically equal to 1 MeV) in corotating interaction regions
British Library Conference Proceedings | 1998
|