Direct observations of the full Dungey convection cycle in the polar ionosphere for southward interplanetary magnetic field conditions

• Main Authors: Q-H Zhang, M Lockwood, JC Foster, S-R Zhang, B-C Zhang, IW Mccrea, J Moen, M Lester, JM Ruohoniemi
• Format: Other Non-Article Part of Journal/Newspaper
• Language: unknown
• Published: 2015
• Subjects: Uncategorized; Dungey convection cycle; EISCAT radar; GPS TEC; Polar cap patches; Tromsø; EISCAT
• Online Access: https://figshare.com/articles/journal_contribution/Direct_observations_of_the_full_Dungey_convection_cycle_in_the_polar_ionosphere_for_southward_interplanetary_magnetic_field_conditions/10140734

Tracking the formation and full evolution of polar cap ionization patches in the polar ionosphere, we directly observe the full Dungey convection cycle for southward interplanetary magnetic field (IMF) conditions. This enables us to study how the Dungey cycle influences the patches' evolution. The patches were initially segmented from the dayside storm enhanced density plume at the equatorward edge of the cusp, by the expansion and contraction of the polar cap boundary due to pulsed dayside magnetopause reconnection, as indicated by in situ Time History of Events and Macroscale Interactions during Substorms (THEMIS) observations. Convection led to the patches entering the polar cap and being transported antisunward, while being continuously monitored by the globally distributed arrays of GPS receivers and Super Dual Auroral Radar Network radars. Changes in convection over time resulted in the patches following a range of trajectories, each of which differed somewhat from the classical twin-cell convection streamlines. Pulsed nightside reconnection, occurring as part of the magnetospheric substorm cycle, modulated the exit of the patches from the polar cap, as confirmed by coordinated observations of the magnetometer at Tromsø and European Incoherent Scatter Tromsø UHF radar. After exiting the polar cap, the patches broke up into a number of plasma blobs and returned sunward in the auroral return flow of the dawn and/or dusk convection cell. The full circulation time was about 3h.