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Particle transport at CME-driven shocks

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Original languageEnglish
Title of host publicationSOLAR WIND TEN
Subtitle of host publicationProceedings of the Tenth International Solar Wind Conference
PublisherAIP PRESS
Pages636-639
Volume679
Publication statusPublished - 1 Sep 2003

Abstract

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.

    Research areas

  • Particle emission solar wind, Planetary bow shocks, interplanetary shocks

ID: 19679927