Effects of the solar cycle on cusp/cleft O+ outflow access to the polar cap and lobes

Details Effects of the solar cycle on cusp/cleft O+ outflow access to the polar cap and lobes Effects of the solar cycle on cusp/cleft O+ outflow access to the polar cap and lobes

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm22a..07l&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM22A-07

Physics

[2731] Magnetospheric Physics / Magnetosphere: Outer, [2736] Magnetospheric Physics / Magnetosphere/Ionosphere Interactions, [2744] Magnetospheric Physics / Magnetotail, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions

Scientific paper

The polar orbit of the CLUSTER satellite is ideal for observing ion outflow from the cusp, and how those ions are transported across the polar cap, and into the lobe. Using the CODIF/CIS instrument, which measures the 3D distributions of the major magnetospheric ion species over the energy range 40 eV to 40 keV, we have developed an automated procedure to identify when tailward streaming O+ are observed on CLUSTER. The database gives the occurrence frequency of the O+ beams, and their flux and energy, density and temperature as a function of position for geomagnetically quiet and storm times. The CLUSTER satellites were launched in 2000, the maximum of solar cycle 23, and have continued to operate as the solar activity has declined to its current deep minimum. In our previous work, we have concentrated on the early years, close to solar maximum, to show how the O+ flux and transport paths depend on the IMF magnitude and orientation, solar wind pressure, and geomagnetic activity. By extending our database into the solar minimum, we will show how the ion outflow characteristics and the ion transport change during the solar cycle.

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