The November 9, 1993, traveling convection vortex event: A case study

On November 9, 1993, at around 1715 UT, a strong and well-structured travel ing convection vortex (TCV) event occurred and was observed by the Magnetom eter Array for Cusp and Cleft Studies (MACCS) and the Canadian Auroral Netw ork for the OPEN Program Unified Study (CANOPUS) magnetometer chains. The G reenland chain, which is located farther to the east, observed only a very weak signature for the same event. We studied the propagation characteristi cs of the two-dimensional vortical TCV current patterns. The TCV event is a series of four vortical currents propagating westward. We found that indiv idual vortices propagate with different speeds. The vortices are created in the early postnoon region. They accelerate as they strengthen, and some de celerate, weaken, and disappear within the 6 hours of magnetic local time o f the field of view of the ground magnetometers. The strongest, main vortex of the event accelerates until it moves out of the field of view and, more than likely, reaches well into the nightside, We studied the correlated so lar wind and IMF signatures as observed by the IMP 8 spacecraft, sitting in the far dawnside and outside the bow shock. We found that the transient cu rrents in the ionosphere are the result of sharp, short-lived pressure puls es hitting the magnetopause during times of quiet and northward IMF that is primarily radial. We find that the pressure pulses are more than likely cr eated just upstream of the bow shock by the interaction of the quasi-parall el shock with IMF orientation changes and are not intrinsic features of the upstream solar wind. We also analyze the transient signatures in the inner magnetosphere by studying the magnetic field data in the GOES 6 and 7 sate llites. We suggest that a series of five successive compression and depress ion peaks in the GOES magnetic field data are well correlated with the set of solar wind pressure pulses. We observe a propagation velocity of the tra nsient event from the GOES 6 spacecraft to the GOES 7 spacecraft that agree s well with the propagation velocities that we calculate from the ground ma gnetometer stations.