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Observations of asymmetries in ionospheric return flow during different levels of geomagnetic activity

Research output: Contribution to journalJournal article

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  • J. P. Reistad
  • N. Ostgaard
  • K. M. Laundal
  • A> Ohma
  • K. Snekvik
  • P. Tenfjord
  • Adrian Grocott
  • Kjellmar Oksavik
  • S.E. Milan
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<mark>Journal publication date</mark>06/2018
<mark>Journal</mark>Journal of Geophysical Research: Space Physics
Issue number6
Volume123
Number of pages14
Pages (from-to)4638-4651
Publication statusPublished
Early online date21/05/18
Original languageEnglish

Abstract

It is known that the magnetic field of the Earth's closed magnetosphere can be highly displaced from the quiet‐day configuration when interacting with the Interplanetary Magnetic Field (IMF), an asymmetry largely controlled by the dawn‐dusk component of the IMF. The corresponding ionospheric convection has revealed that footprints in one hemisphere tend to move faster to reduce the displacement, a process we refer to as the restoring of symmetry. Although the influence on the return flow convection from the process of restoring symmetry has been shown to be strongly controlled by the IMF, the influence from internal magnetospheric processes has been less investigated. We use 14 years of line‐of‐sight measurements of the ionospheric plasma convection from the Super Dual Auroral Radar Network (SuperDARN) to produce high‐latitude convection maps sorted by season, IMF, and geomagnetic activity. We find that the restoring symmetry flows dominate the average convection pattern in the nightside ionosphere during low levels of magnetotail activity. For increasing magnetotail activity, signatures of the restoring symmetry process become less and less pronounced in the global average convection maps. We suggest that tail reconnection acts to reduce the asymmetric state of the closed magnetopsphere by removing the asymmetric pressure distribution in the tail set up by the IMF By interaction. During active periods the nightside magnetosphere will therefore reach a more symmetric configuration on a global scale. These results are relevant for better understanding the dynamics of flux‐tubes in the asymmetric geospace, which is the most common state of the system.