Dual Reversed Convection and Magnetospheric Reconfiguration Under Strongly Northward IMF Conditions (Invited)

Details Dual Reversed Convection and Magnetospheric Reconfiguration Under Strongly Northward IMF Conditions (Invited) Dual Reversed Convection and Magnetospheric Reconfiguration Under Strongly Northward IMF Conditions (Invited)

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm34a..07l&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM34A-07

Physics

[2723] Magnetospheric Physics / Magnetic Reconnection, [2760] Magnetospheric Physics / Plasma Convection, [2776] Magnetospheric Physics / Polar Cap Phenomena, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions

Scientific paper

We present a case study of ionospheric and magnetospheric response to a prolonged interval of strongly northward IMF along with enhanced solar wind dynamic pressure on November 9, 2004. Comprehensive space and ground based observations are examined to investigate global electrodynamic properties of the ionosphere and magnetosphere under northward IMF conditions, including the Cluster satellites located near the high-altitude southern cusp region, the low-altitude DMSP and Fast spacecraft, and ground radar network and magnetometer chains. Global patterns of high-latitude ionospheric convection obtained from the assimilative mapping of ionospheric electrodynamics (AMIE) procedure based on various ground and low-altitude spacecraft measurements show the formation of reserved ionospheric convection in both northern and southern hemispheres simultaneously for nearly 2 hours. Global MHD simulations are also carried out to investigate the physical processes involved in the solar wind-magnetosphere-ionosphere interaction, particularly, the reconnection configuration near the magnetopause, the transport of mass and energy, and the coupling between the magnetosphere and the ionosphere during northward IMF. Cluster observations indicate that multiple magnetopause crossings had been encountered by the spacecraft due to variations in the solar wind dynamic pressure, and the plasma characteristics are consistent with magnetic reconnection taking place tailward of the spacecraft location.

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