HR: 0800h
AN: SM31B-1227    [Abstracts]
TI: Interpretation of Automated Forward Modeling Parameters for Sawtooth Events and Steady Magnetospheric Convection
AU: * Connors, M
EM: martinc@athabascau.ca
AF: Athabasca University, 1 University Drive, Athabasca, AB T9S 3A3 Canada
AU: McPherron, R L
EM: rmcpherron@igpp.ucla.edu
AF: University of California, Los Angeles, Institute of Geophysics and Planetary Physics, Los Angeles, CA 90095-1567 United States
AB: Automated Forward Modeling (AFM) is an inversion technique based on magnetic data alone, which can indicate physical parameters associated with electrojets. From perturbations along a meridian, the total electric current crossing the meridian may be determined, as well as the latitudes between which it flowed. The technique is based on nonlinear optimization of the parameters of a forward model. It is possible to compare model output to the original input to ensure that the routine has functioned well and that output parameters are reliable and presumably have physical meaning. Characteristic behaviors of substorms are readily seen in modeling output: the current strengthens rapidly and considerably at an expansive phase onset, following a growth phase during which the electrojet borders move equatorward, usually with some strengthening of current. At onset the poleward border is often seen to move poleward rapidly. Poleward border activity may be noted then and also at other times. After an onset, the recovery phase is often marked by a retreat of the equatorward border, indicating the well-known shrinkage of the auroral oval. These complete cycles of activity are absent in steady magnetospheric convection (SMC) and sawtooth events. Our output parameters can be diagnostic of onsets and useful in determining their location and role in SMC. Sawtooth events have many of the characteristics of expansive phase onsets, but maximum poleward expansion of the poleward border is followed by equatorward movement reminiscent of a growth phase. Since this is correlated with the interplanetary magnetic field remaining southward, the difference from common expansive phase phenomenology may simply be the lack of a recovery phase. For SMC, onset-like activity appears to be concentrated at the poleward border and of small magnitude compared to the overall convection electrojets. The activity is reminiscent of poleward border intensifications.
DE: 2740 Magnetospheric configuration and dynamics
DE: 2753 Numerical modeling
DE: 2788 Storms and substorms
DE: 2794 Instruments and techniques
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting