Acceleration of O+ from the cusp to the lobe

Details Acceleration of O+ from the cusp to the lobe Acceleration of O+ from the cusp to the lobe

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm33b1897l&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM33B-1897

Physics

[2736] Magnetospheric Physics / Magnetosphere/Ionosphere Interactions, [2740] Magnetospheric Physics / Magnetospheric Configuration And Dynamics, [2744] Magnetospheric Physics / Magnetotail, [2760] Magnetospheric Physics / Plasma Convection

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 lobes. 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 cusp outflow is dispersed according to its velocity as it is transported to the tail, due to the velocity filter effect. Thus changes in beam velocity over the Cluster orbit may result simply from passing through different spatial regions, and do not necessarily indicate acceleration. To determine if there is any acceleration, the flux of the O+ observed at a particular energy must be compared with initial flux over the cusp at that same energy. By performing these comparisons, we will determine how much acceleration is required to explain the observed O+ with high energy in the tail lobes at ~-20 Re.

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