Comparison of the Charge States of Energetic Ions and Solar Wind in Co-Rotating Interaction Regions

Details Comparison of the Charge States of Energetic Ions and Solar Wind in Co-Rotating Interaction Regions Comparison of the Charge States of Energetic Ions and Solar Wind in Co-Rotating Interaction Regions

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh52b..04m&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH52B-04

Physics

2102 Corotating Streams, 2114 Energetic Particles, Heliospheric (7514), 2164 Solar Wind Plasma

Scientific paper

The ionic charge states of energetic C, O, Ne, Mg, and Fe have been observed in several recurrences of co-rotating interaction region (CIR) during solar maximum in 1999 and 2000 with ACE SEPICA. Except for a small, but noticeable, contribution of singly charged Ne, the mean charge states of the energetic ions in these events have been found to be similar to those observed in CME related energetic particle populations and in the solar wind. Therefore, the charge states of heavy ions appear to be a good tracer for the potential solar wind source distributions. We compare the charge states of the energetic ions in the CIRs with the charge states of heavy solar wind ions separated into fast and slow compressed and undisturbed solar wind for each of the CIR recurrences, as observed with ACE SWICS. Small, but noticeable event-to-event variations in the charge states of the energetic ions have been observed that are consistent among the different species, which we compare with variations in the adjacent solar wind regions. We will also analyze whether the charge states are compatible with the idea that a substantial fraction of energetic CIR ions may be accelerated out of the fast solar wind.

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