High-Latitude Ionospheric Upwelling as a Function of Cross-Cap Potential and Solar Wind Pressure

Details High-Latitude Ionospheric Upwelling as a Function of Cross-Cap Potential and Solar Wind Pressure High-Latitude Ionospheric Upwelling as a Function of Cross-Cap Potential and Solar Wind Pressure

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsa33a1057c&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SA33A-1057

Physics

2431 Ionosphere/Magnetosphere Interactions (2736), 2435 Ionospheric Disturbances, 2437 Ionospheric Dynamics, 2441 Ionospheric Storms (7949), 2475 Polar Cap Ionosphere

Scientific paper

We have examined characteristics of the vertical ion flux of thermal O+ in the topside high-latitude ionosphere from under a variety of solar activity conditions from 1998 to 2002 using measurements of the vertical ion drift and ion number density made by the DMSP F13 spacecraft. During geomagnetically quiet times typical upward fluxes of approximately 108--109 cm-2s-1 are observed in the auroral zones with somewhat smaller downward fluxes in the polar caps. Immediately following the onset of a geomagnetic storm upward fluxes reach and sometimes exceed 1010 cm-2s-1 and are observed with vertical velocities of 500--1500 m s-1. At the same time downward fluxes at the higher latitudes reach unusually high values of 109 cm-2s-1. Separately integrating the upwards and downwards fluxes over the high-latitude region (auroral zone and polar cap) for each spacecraft pass allows for the observation of total upflow/downflow during various geomagnetic activity levels. Analysis of these integrated fluxes indicates a positive correlation of the upward and downward flux magnitudes to the polar cross-cap potential. In addition, the magnitude of the upwelling flux increases by approximately a factor of 2 during the change from conditions of low solar wind dynamic pressure to high dynamic pressure. Solar cycle effects will also be discussed.

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