Low Energy Charged Particles in the High Latitude Heliosphere: Comparing Solar Maximum to Solar Minimum

Details Low Energy Charged Particles in the High Latitude Heliosphere: Comparing Solar Maximum to Solar Minimum Low Energy Charged Particles in the High Latitude Heliosphere: Comparing Solar Maximum to Solar Minimum

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh41a..08m&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH41A-08

Physics

2114 Energetic Particles, Heliospheric (7514), 2118 Energetic Particles, Solar, 2162 Solar Cycle Variations (7536)

Scientific paper

The structure of the inner heliosphere that was delineated by the energetic charged particle populations (electrons and ions) during the recent Ulysses fast latitude scan during solar maximum conditions is found to be very different from that measured during a similar latitudinal transit in solar minimum conditions. Measurements made by the Heliosphere Instrument for Spectra, Composition and Anisoptropy at Low Energies (HI-SCALE; electrons ~50-1000 keV and ions ~50 keV-10000 keV/nucl) during solar maximum show that the inner heliosphere was populated at all latitudes, and with varying spatial scales, by particles largely originating from active solar regions. During solar minimum the major particle populations were confined to the near equatorial solar current sheet. The relative energetic ion (Z>2) abundances throughout the inner heliosphere were also substantially different, a result of the dominance in the inner heliosphere of solar-produced particles during solar maximum and the dominance of anomalous cosmic ray ions (especially O) and interplanetary accelerated particles during solar minimum. The H/He abundance ratios are nearly a factor of ten larger during solar maximum conditions at all heliolatitudes, showing the importance of a dominant solar source during this epoch. The ratios of the HI-SCALE ion abundances in the fast latitude scan during solar maximum are compared to measurements of ions made during the same time interval with a similar instrument (EPAM) on the ACE spacecraft in the ecliptic plane near 1 AU and show significant variations with time and spatial location. However, there are several intervals of time following solar maximum activity, including at latitudes as high as 80 degrees, during which the ion abundances and the electron fluxes at both locations are nearly identical. These intervals demonstrate that at times particle reservoirs (which are found to persist for nearly a solar rotation), can be established in the inner heliosphere and have volumes ranging from ~40 to ~ 150AU3.

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