Super dual auroral radar network radar imaging of dayside high-latitude convection under northward interplanetary magnetic field: Toward resolving the distorted two-cell versus multicell controversy

Details Super dual auroral radar network radar imaging of dayside high-latitude convection under northward interplanetary magnetic field: Toward resolving the distorted two-cell versus multicell controversy Super dual auroral radar network radar imaging of dayside high-latitude convection under northward interplanetary magnetic field: Toward resolving the distorted two-cell versus multicell controversy

Oct 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jgr...10019661g&link_type=abstract

Journal of Geophysical Research, Volume 100, Issue A10, p. 19661-19674

Physics

41

Magnetospheric Physics: Electric Fields, Magnetospheric Physics: Plasma Convection, Magnetospheric Physics: Magnetospheric Configuration And Dynamics

Scientific paper

Data from the Kapuskasing and Saskatoon radars of the evolving Super Dual Auroral Radar Network (SuperDARN) HF radar network have been analyzed to study the two-dimensional structure and dynamics of dayside high-latitude ionospheric convection under northward interplanetary magnetic field (IMF) conditions. A period extending from 1600 to 2030 UT (~0900-1330 MLT) on January 10, 1994, was examined. During this interval, magnetic field data were available from the IMP 8 satellite and indicated moderately stable northward IMF conditions. For the first few hours of observation the By component of the IMF was positive, reasonably steady, and approximately twice the magnitude of Bz. During this interval, the high-latitude convection images obtained with the SuperDARN radars were very similar to the distorted two-cell convection maps for positive By as presented by Heppner and Maynard (1987). At ~1840 UT, a decrease in By in association with an increase in Bz, led to an extended period with By~Bz. During this second interval the convection patterns were highly variable and even chaotic.
Finally, a sharp decrease in the By component at 1914 UT, probably in association with a rotational discontinuity in the solar wind, led to an extended period with By<

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