High-Latitude Plasma Convection as a Function of Solar Wind and IMF Using a Simple Parameterization

Details High-Latitude Plasma Convection as a Function of Solar Wind and IMF Using a Simple Parameterization High-Latitude Plasma Convection as a Function of Solar Wind and IMF Using a Simple Parameterization

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm31b0782b&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SM31B-0782

Physics

2463 Plasma Convection, 2736 Magnetosphere/Ionosphere Interactions, 2760 Plasma Convection

Scientific paper

A simple parameterization of high-latitude ionospheric plasma convection patterns has been developed to study the relationship of the convection patterns to the speed and density of the solar wind and the interplanetary magnetic field (IMF). The parameterization includes the overall size of the convection pattern, the total potential drop, the orientation of the pattern, and the relative sizes of the dawn and dusk convection cells. The spherical harmonic fitting analysis of Ruohoniemi and Baker [1998] was applied to two years (1999, 2000) of SuperDARN HF-Radar data from the northern hemisphere. Solar Wind and IMF data were take from the definitive ACE key parameter data. Linear regression analysis was applied to determine the relationship of the convection pattern parameters to various combinations of solar wind and IMF parameters. The polar cap potential drop was found to be most strongly correlated to vBz, but a weaker correlation to v*abs(By) was also noted. The orientation of the convection pattern was well correlated with either By alone or the IMF clock angle. Ruohoniemi, J. M., and K. B. Baker, Large-scale imaging of high-latitude convection with SuperDARN HF-radar observations, J. Geophys. Res., 103, 20,797-20,811, 1998.

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