Interplanetary Shock Source Population: Hybrid Simulations and ACE Observations

Details Interplanetary Shock Source Population: Hybrid Simulations and ACE Observations Interplanetary Shock Source Population: Hybrid Simulations and ACE Observations

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh43a..07k&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH43A-07

Other

2114 Energetic Particles, Heliospheric (7514), 2118 Energetic Particles, Solar, 2139 Interplanetary Shocks, 2159 Plasma Waves And Turbulence

Scientific paper

Recently, we started using large-scale hybrid (kinetic ions, electron fluid) simulations to describe and deliver the pertinent characteristics of the energetic shock ion populations to large-scale transport models, such as the CISM SEP model. Such transport models decouple the scales and processes of ion acceleration at interplanetary shocks (ISs) from those of further heliospheric transport by assuming that a defined "SEP source" can be associated with the shock. This approach is more easily put into reality in some regions of parameter space than in others. In particular, shock acceleration at weak and/or quasi-perpendicular shocks remains poorly understood. In an effort to remedy this situation, we are comparing in situ ACE observations of energetic ions at ISs with our hybrid simulations. Such comparisons also provide a validation mechanism to source and transport models. We discuss the role of seed particles and the question of which portion of a non-Maxwellian solar wind distribution contributes most efficiently to highly-energized ions.

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