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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 33, issue 10
Ann. Geophys., 33, 1271–1283, 2015
https://doi.org/10.5194/angeo-33-1271-2015
© Author(s) 2015. This work is distributed under
the Creative Commons Attribution 3.0 License.

Special issue: Dynamic processes in geospace

Ann. Geophys., 33, 1271–1283, 2015
https://doi.org/10.5194/angeo-33-1271-2015
© Author(s) 2015. This work is distributed under
the Creative Commons Attribution 3.0 License.

Regular paper 16 Oct 2015

Regular paper | 16 Oct 2015

The relationship between plasmapause, solar wind and geomagnetic activity between 2007 and 2011

G. Verbanac1, V. Pierrard2,3, M. Bandić4, F. Darrouzet2, J.-L. Rauch5, and P. Décréau5 G. Verbanac et al.
  • 1Department of Geophysics, University of Zagreb, Zagreb, Croatia
  • 2Belgian Institute for Space Aeronomy (Space Physics and STCE), 3 Av. Circulaire, 1180 Brussels, Belgium
  • 3Université Catholique de Louvain, TECLIM, Earth and Life Institute, Place Louis Pasteur 3 bte L4.03.08, 1348 Louvain-La-Neuve, Belgium
  • 4Preziosastr. 15a, 81927 München, Germany
  • 5Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Orléans, France

Abstract. Taking advantage of the Cluster satellite mission and especially the observations made by the instrument WHISPER to deduce the electron number density along the orbit of the satellites, we studied the relationships between the plasmapause positions (LPP) and the following LPP indicators: (a) solar wind coupling functions Bz (Z component of the interplanetary magnetic field vector, B, in GSM system), BV (related to the interplanetary electric field; B is the magnitude of the interplanetary magnetic field vector, V is solar wind velocity), and dΦmp/dt (which combines different physical processes responsible for the magnetospheric activity) and (b) geomagnetic indices Dst, Ap and AE. The analysis is performed separately for three magnetic local time (MLT) sectors (Sector1 – night sector (01:00–07:00 MLT); Sector2 – day sector (07:00–16:00 MLT); Sector3 – evening sector (16:00–01:00 MLT)) and for all MLTs taken together. All LPP indicators suggest the faster plasmapause response in the postmidnight sector. Delays in the plasmapause responses (hereafter time lags) are approximately 2–27 h, always increasing from Sector1 to Sector3. The obtained fits clearly resolve the MLT structures. The variability in the plasmapause is the largest for low values of LPP indicators, especially in Sector2. At low activity levels,LPP exhibits the largest values on the dayside (in Sector2) and the smallest on the postmidnight side (Sector1). Displacements towards larger values on the evening side (Sector3) and towards lower values on the dayside (Sector2) are identified for enhanced magnetic activity. Our results contribute to constraining the physical mechanisms involved in the plasmapause formation and to further study the still not well understood related issues.

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Using Cluster data, we develop plasmapause Lpp models parameterized by solar wind coupling functions and geomagnetic activity indices. We show that the Lpp response to the changes in the interplanetary conditions depends on the magnetic local time. The faster plasmapause response is observed in the post-midnight sector. At low activity, Lpp exhibits the largest values on the dayside. For enhanced activity, displacements towards larger values on the evening side are identified.
Using Cluster data, we develop plasmapause Lpp models parameterized by solar wind coupling...
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