A Comparison of Elemental Abundance Ratios in SEP Events in Fast and Slow Solar Wind Regions

Details A Comparison of Elemental Abundance Ratios in SEP Events in Fast and Slow Solar Wind Regions A Comparison of Elemental Abundance Ratios in SEP Events in Fast and Slow Solar Wind Regions

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh43c..01k&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH43C-01

Physics

2101 Coronal Mass Ejections (7513), 2114 Energetic Particles (7514)

Scientific paper

The solar energetic (E > 1 MeV) particles (SEP) observed in gradual events at 1 AU are generally assumed to be accelerated from ambient suprathermal particles. If so, then the elemental abundances of SEPs produced in fast wind regions might be systematically distinguished from the abundances of those from slow wind regions. We look for these differences using the Mg/Ne ratios in a large number of SEP events from the past solar cycle. The solar wind regions are characterized by O7/O6 ratios and by the three-component wind stream classification of Richardson et al. (JGR, 2002). The Mg/Ne ratio provides a low/high first ionization potential (FIP) element ratio with comparable particle rigidities to minimize propagation effects. Our initial survey shows no significant differences in the 5-10 MeV/nucleon range for fast and slow wind SEP events. This result supplements the earlier finding that SEP events are observed frequently in fast wind and are not associated with unusually higher CME speeds, although the higher Alfven and solar wind flow speeds in fast wind regions should mitigate against the production of CME-driven shocks in those regions. We discuss the implications of our results for shock seed populations and cross-field propagation. AJT was supported by the Office of Naval Research and NASA DPR NNG06EC55I.

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