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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 27, issue 5
Ann. Geophys., 27, 1951–1960, 2009
https://doi.org/10.5194/angeo-27-1951-2009
© Author(s) 2009. This work is distributed under
the Creative Commons Attribution 3.0 License.

Special issue: Ninth International Conference on Substorms (ICS9)

Ann. Geophys., 27, 1951–1960, 2009
https://doi.org/10.5194/angeo-27-1951-2009
© Author(s) 2009. This work is distributed under
the Creative Commons Attribution 3.0 License.

  04 May 2009

04 May 2009


Development of substorm bulges during different solar wind structures

I. V. Despirak1, A. A. Lubchich1, A. G. Yahnin1, B. V. Kozelov1, and H. K. Biernat2 I. V. Despirak et al.
  • 1Polar Geophysical Institute, Apatity, Russia
  • 2Space Research Institute, Graz, Austria

Abstract. Using data from WIND spacecraft, we investigated the difference in substorm bulge development during different types of solar wind flow: solar wind recurrent streams (RS), corotating interaction regions (CIR), magnetic clouds (MC), and the region of interaction of magnetic clouds with undisturbed solar wind (Sheath). The RS/CIR and MC/Sheath structures were examined for the periods December 1996–July 1997; January 2000–December 2000; October 2001. All available auroral substorms observed by the Ultra Violet Imager onboard the Polar spacecraft during these periods were studied. It is shown that the largest latitudinal and longitudinal sizes of the auroral bulge expansions are during CIR and Sheath intervals. We found a difference in auroral bulge parameters for MC- and RS-associated substorms. In contrast to substorms associated with RS, the latitudinal size of the auroral bulge during MC is smaller, but longitudinal size is larger. As consequence, the ratio between longitudinal and latitudinal sizes for MC-associated substorms is also larger. We suggest that the latter feature is explained by different configuration of the near-Earth magnetotail during RS and MC.

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