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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 28, issue 4
Ann. Geophys., 28, 1003–1012, 2010
https://doi.org/10.5194/angeo-28-1003-2010
© Author(s) 2010. This work is distributed under
the Creative Commons Attribution 3.0 License.
Ann. Geophys., 28, 1003–1012, 2010
https://doi.org/10.5194/angeo-28-1003-2010
© Author(s) 2010. This work is distributed under
the Creative Commons Attribution 3.0 License.

  22 Apr 2010

22 Apr 2010

Average auroral configuration parameterized by geomagnetic activity and solar wind conditions

S. E. Milan1, T. A. Evans1, and B. Hubert2 S. E. Milan et al.
  • 1Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK
  • 2Laboratory of Planetary and Atmospheric Physics, University of Liége, Liége, 4000 Belgium

Abstract. Average proton and electron auroral images are compiled from three years of observations by the IMAGE spacecraft, binned according to concurrent KP and upstream solar wind conditions measured by the ACE spacecraft. The solar wind parameters include solar wind velocity, density, and pressure, interplanetary magnetic field (IMF) magnitude and orientation, and an estimate of the magnetopause reconnection rate. We use both (a) the overall variation in brightness in the images and (b) the variation in location of the aurorae with respect to the binning parameters to determine which parameters best order the auroral response. We find that the brightness varies by a factor of ~50 with KP, a similar amount with estimated dayside reconnection voltage, ~15 with the IMF, ~3 with solar wind density, ~2 with solar wind velocity, and ~5 with pressure. Clearly, geomagnetic activity as measured by KP and auroral dynamics are closely associated. In terms of the solar wind-magnetosphere coupling that drives auroral dynamics, the IMF is of paramount importance in modulating this, with solar wind speed and density playing a lesser role. Dayside reconnection voltage, derived from the solar wind velocity and IMF magnitude and orientation, orders the data almost as well as KP, though we find a plateau in the auroral response between voltages of 100 and 150 kV. We also discuss changes in configuration and overall size of the average auroral oval with upstream conditions.

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