Challenges for Modeling Acceleration and Transport in Solar Energetic Particle Events

Details Challenges for Modeling Acceleration and Transport in Solar Energetic Particle Events Challenges for Modeling Acceleration and Transport in Solar Energetic Particle Events

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh62a..03t&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH62A-03

Other

2118 Energetic Particles, Solar, 7513 Coronal Mass Ejections, 7514 Energetic Particles (2114), 7519 Flares, 7807 Charged Particle Motion And Acceleration

Scientific paper

Shocks, driven by fast coronal mass ejections (CMEs), are believed to be the primary accelerator of energetic particles in large, so-called "gradual" solar particle events. Thus far in Cycle 23, instruments on ACE, Wind, SOHO, and IMP8 have provided detailed observations of the energy spectra, composition, and temporal evolution of nearly 50 large events in which the differential proton intensity at ~20 MeV exceeded galactic cosmic ray levels by a factor of more than 104. These events exhibit a large range of variability in all of their characteristics. Some of this variability is reasonably well understood in terms of familiar notions about shock acceleration, source-plasma composition, and particle transport. For other aspects we appear to have a qualitative understanding that is not yet bolstered by detailed quantitative modeling. However, many observed characteristics, such as spectral variability among elemental species, clearly challenge our present understanding. We will review these new challenges and speculate about the physics issues that must be addressed in future modeling efforts.

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