Modeling Field Line Resonances in the Inner Plasmasphere with the Field Line Interhemispheric Plasma Model

Details Modeling Field Line Resonances in the Inner Plasmasphere with the Field Line Interhemispheric Plasma Model Modeling Field Line Resonances in the Inner Plasmasphere with the Field Line Interhemispheric Plasma Model

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsa41b1729m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SA41B-1729

Physics

[2730] Magnetospheric Physics / Magnetosphere: Inner, [2768] Magnetospheric Physics / Plasmasphere, [2772] Magnetospheric Physics / Plasma Waves And Instabilities

Scientific paper

Equatorial plasma mass density in the Inner Magnetosphere of the Earth has been traditionally derived from measurements of Field Line Resonances from pairs of ground magnetometers closely spaced in latitude. The full plasma mass density along the flux tube can be determined using such measurements in an inversion of the Field Line Resonance Equation. Cummings et al [1969] developed the Field Line Resonance equation and numerically solved for the Field Line Resonances by assuming a power law distribution that varied with the geocentric distance from the equatorial crossing point of the field lines and a dipole model for the Earth's magnetic field. So far all numerical solutions of the Field Line Resonance Equation use some form of a power law distribution of the mass density along the field line, that depends on the magnetic field model, typically assumed to be a dipole, with only one recent work exploring deviations from a dipole magnetic field. Another fundamental assumption in the solution of the Field Line Resonance Equation is that of perfectly conducting, flat ionospheres as the two boundaries of the field line. While this assumption is considered valid for L values greater than 2, recent works have found it to be invalid for L values of 3 or less. In the present paper we solve the Field Line Resonance Equation for L values less than 3.5 using a three dimensional ionosphere, and without assuming a power law for the mass density distribution along the field line. Instead we use plasma mass density data from the Field Line Interhemispheric Plasma (FLIP) model to numerically solve the Field Line Resonance Equation for the eigenfrequencies. We also examine how the resonance frequencies vary as a function of the driving parameters. Finally we examine two events in which we compare the derived frequencies with measurements from the SAMBA magnetometer array.

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