It has been commonly accepted that in large solar energetic particle (SEP) events, particles are often accelerated to MeV energies (and perhaps up to GeV energies) at shock waves driven by coronal mass ejections (CMEs). As a CME-driven shock propagates, expands and weakens, particles accelerated diffusively at the shock can escape upstream and downstream into the interplanetary medium. These escaping energized particles then propagate along the interplanetary magnetic field, experiencing only weak scattering from fluctuations in the interplanetary magnetic field (IMF). In this paper, we concentrate on the transport of energetic particles escaping from a CME-driven shock using a Monte-Carlo approach. This work, along with our previous work on particle acceleration at shocks, allows us to investigate the characteristics (intensity profiles, spectra, angular distribution, particle anisotropies) of high-energy particles arriving at various distances from the sun and form an excellent basis with which to interpret observations of high-energy particles made at 1 AU by ACE and WIND.
|Title of host publication||SOLAR WIND TEN|
|Subtitle of host publication||Proceedings of the Tenth International Solar Wind Conference|
|Publication status||Published - 1 Sep 2003|
- Particle emission solar wind
- Planetary bow shocks
- interplanetary shocks