Field Line Resonance Measurements in the Inner Magnetosphere During Large Storms: Implications for Convection and Depletion

Details Field Line Resonance Measurements in the Inner Magnetosphere During Large Storms: Implications for Convection and Depletion Field Line Resonance Measurements in the Inner Magnetosphere During Large Storms: Implications for Convection and Depletion

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsa51d1977d&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SA51D-1977

Physics

[2700] Magnetospheric Physics

Scientific paper

Field Line Resonances (FLRs) have been shown to be an effective way to remote sense plasmaspheric mass density. In the outer plasmasphere the mass density is modeled well by a power-law distribution and solutions have been tabulated that allow the direct conversion between resonance frequency and mass density. In the inner plasmasphere, for L<3, plasma density is not modeled by a power law and the resonance equation must be solved directly using a model plasma density. We use the time-dependent Field Line Interhemispheric Plasma (FLIP) model and solve the resonance equation with a finite element method. We compare the solutions with FLR measurements from several magnetometer chains in both the northern and southern hemisphere in the American sector, South American Meridional B-field Array (SAMBA), Magnetometers along the Eastern Atlantic Seaboard for Undergraduate Research and Education (MEASURE), and Mid-continent Magnetoseismic Chain (McMAC). During quiet periods the FLIP model and the observations are in good agreement. During a large storm we find significant differences between the FLIP model and observations. We attribute this difference to the fact that the FLIP model does not automatically incorporate the effects of strong convection, such as a change in flux tube volume (and location), nor the depletion of plasma from the flux tube. In the present study we incorporate these effects realistically and use comparison with observations to estimate their importance in driving the inner plasmasphere during large storms.

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