Ionospheric Response to the Changes in the Interplanetary Magnetic Field (IMF) Bz Under Strong Positive IMF By Conditions, as Seen using SuperDARN and PolarDARN Radars.

Details Ionospheric Response to the Changes in the Interplanetary Magnetic Field (IMF) Bz Under Strong Positive IMF By Conditions, as Seen using SuperDARN and PolarDARN Radars. Ionospheric Response to the Changes in the Interplanetary Magnetic Field (IMF) Bz Under Strong Positive IMF By Conditions, as Seen using SuperDARN and PolarDARN Radars.

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm13b1322c&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM13B-1322

Other

2463 Plasma Convection (2760), 2721 Field-Aligned Currents And Current Systems (2409), 2723 Magnetic Reconnection (7526, 7835), 2736 Magnetosphere/Ionosphere Interactions (2431), 2790 Substorms

Scientific paper

The interplanetary magnetic field (IMF) is known to have a profound influence on the ionospheric convection pattern at high latitudes. Thus, when the IMF has a dominant southward (Bz) component, the convection over the central polar cap is anti-sunward and closes through the dawn and dusk sectors to produce a familiar 2-cell convection pattern. For strong northward IMF conditions, the pattern is thought to break into four cells, with sunward convection taking place over the noon sector of the polar cap. For strong IMF By conditions the standard 2-cell convection pattern is believed to become asymmetric and/or to rotate from its basic alignment with the noon-to- midnight meridian to a more dusk-to-dawn or dawn-to-dusk alignment. With the help of the new PolarDARN radar in combination with other SuperDARN radar data, we have been able to observe changes occurring deep into the polar cap during a period of strong sustained positive IMF By, when the Bz component was always less than 20% of the By component in magnitude. The basic shape of the convection pattern was highly reminiscent of the Heppner-Maynard `BC' convection pattern predicted for strong positive By conditions ( Heppner and Maynard, JGR, 92, 4467, 1987). We note that we observed very clear changes in the convection pattern as Bz changed signs, with a distinct sub-cell on the evening side being present while the IMF Bz component was greater than zero. The sub-cell completely vanished when the Bz component changed sign. These variations were unexpected in view of the relatively small IMF Bz magnitudes involved. Interestingly enough, this feature would have been missed, had the PolarDARN radar data not been added to the data obtained with the rest of the SuperDARN radars. We will discuss the implications of our findings for our understanding of ionospheric/magnetospheric convection in response to solar wind inputs.

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