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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 15, issue 8
Ann. Geophys., 15, 967–983, 1997
© European Geosciences Union 1997
Ann. Geophys., 15, 967–983, 1997
© European Geosciences Union 1997

  31 Aug 1997

31 Aug 1997

Auroral precipitation fading before and at substorm onset: ionospheric and geostationary signatures

K. Kauristie1, T. I. Pulkkinen1, A. Huuskonen1, R. J. Pellinen1, H. J. Opgenoorth2, D. N. Baker3, A. Korth4, and M. Syrjäsuo1 K. Kauristie et al.
  • 1Finnish Meteorological Institute, Department of Geophysics, Helsinki, Finland
  • 2Swedish Institute of Space Physics, Uppsala, Sweden (also: visiting Prof. at Finnish Meteorological Institute)
  • 3Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
  • 4Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany

Abstract. Rapid fading of auroral activity a few minutes before substorm breakup has earlier been analyzed in case-studies. Here we report on a study in which all-sky camera (ASC) and magnetic data over 3 years were examined to find breakups that were accompanied by a preceding fading. To illustrate typical features of the fading effect we analyze three events in detail and discuss seven other events to find the spatial and temporal behavior of the fading and the global conditions favoring this phenomenon, which is not associated with every breakup. In these ten events the precipitation diminished typically for about 2 min and a local breakup followed after 2–3 min. Usually the arc which broke up had faded earlier. Comparison with geostationary electron flux recordings shows that in many cases the global onset had already taken place when the fading was recorded at a different longitude. Thus fading is not just a growth-phase phenomenon as often thought, but can also appear as a precursor of the approaching auroral bulge. The AE index and solar-wind data reveal that the fading has a tendency to take place during magnetically disturbed conditions caused by continuous energy input from the solar wind. Furthermore, while a widely recognized phenomenon, we have found that the fading prior to breakup is not a very common feature in the spatio-temporal scale of auroral ASC recordings. In many cases the deepness of the fading had a longitudinal dependence, which leads to the suggestion that this phenomenon is related to azimuthal gradients in the tail magnetic field and/or plasma pressure. Possible scenarios causing fading both before and after the onset are discussed based on a few previously presented theoretical auroral-arc models.

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