Physics
Scientific paper
Sep 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..719..249j&link_type=abstract
PHYSICS OF THE OUTER HELIOSPHERE. AIP Conference Proceedings, Volume 719, pp. 249-259 (2004).
Physics
3
Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind
Scientific paper
Observations of cosmic rays and other energetic charged particles in the heliosphere over the past decade have created new challenges to the standard theoretical paradigms for energetic-particle transport. Certainly, some of these will be resolved using the standard Parker (diffusive) transport equation applied to increasingly sophisticated models of heliospheric phenomena. For example, we can apparently understand the modulation of galactic cosmic rays and the acceleration and transport of galactic cosmic rays in terms of this paradigm. Cosmic-ray reaction back on the plasma can also fit into this paradigm. However, it is also becoming increasingly clear that in some situations the diffusion approximation is not strictly valid. The scattering mean free paths may be large or there are significant anisotropies. For example, observations of solar energetic-particle events show non-diffusive effects, particularly in the early phases. Recently observed enhancements on Voyager 1, attributed to the proximity of the solar-wind termination shock, show large anisotropies. In the inner heliosphere, the transport mean-free paths are comparable to the characteristic macroscopic scales, which again makes diffusion models inaccurate. In this overview, the diffusion approximation and more-general treatments of particle transport are compared. It is concluded that even where the diffusion approximation is not strictly valid, it can be a useful guide to the more complete and complex models.
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