Spatially Resolved Substorm Dynamical Model with Internal and External Substorm Triggers

Details Spatially Resolved Substorm Dynamical Model with Internal and External Substorm Triggers Spatially Resolved Substorm Dynamical Model with Internal and External Substorm Triggers

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsm52b..07h&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SM52B-07

Physics

6939 Magnetospheric Physics, 6944 Nonlinear Phenomena, 7827 Kinetic And Mhd Theory, 7859 Transport Processes

Scientific paper

A spatially-resolved nonlinear dynamics model of the coupled solar wind driven magnetosphere-ionosphere system is developed for the purpose of determining the electrical power flow from the solar wind through the nightside magnetosphere into the ionosphere. The model is derived from Maxwell equations and nonlinear plasma dynamics and focuses on the key conservation laws of mass, charge and energy in the power transfer elements in this complex dynamical system. The models has numerous feedback and feedforward loops for six forms of the distributed energy storage in the M-I system. In contrast to neural networks, the model delineates physically realizable time ordered sequence of energetic events in substorm dynamics. Three types of energy releases are observed in the substorm data and studied with the model. Type I events occur for solar wind conditions that lead to the creation of a near Earth neutral line (NENL) in the geomagnetic tail. Other solar wind conditions lead dominantly to the onset of convection in flux tubes with foot points in the auroral region that produced enhanced field aligned currents (FACs) closing in the ionosphere. These are the type II and type III events. In type II events a sudden northward turning of the IMF produces a transient mis-alignment of the pressure gradient with the gradient of the flux volumes as in the Lyons model. Large transient substorm current wedge and auroral region 1 sense currents are driven by the steep near-Earth pressure gradient in these events type II events. In type III events the slower evolving IMF field directly drives the nightside M-I system. This is the directly driven auroral substorm. We use physics-based filters to classify events in historical databases, and we use the 2-1/2D transport model to simulate the events for model solar wind inputs. The results of the research stress the need for more accurate determinations of the day-side magnetopause arrival times of structures in the solar wind required for space weather forecasting and the role of competing substorm triggering mechanisms.

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