Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsm12a0457s&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #SM12A-0457
Physics
2407 Auroral Ionosphere (2704), 2431 Ionosphere/Magnetosphere Interactions (2736), 2704 Auroral Phenomena (2407), 2736 Magnetosphere/Ionosphere Interactions
Scientific paper
Under the assumption of a vertical magnetic field, the wave dispersion for plasma waves splits into right- and left-hand circularly polarized waves. At frequencies above 0.1 Hz the waves have a profile consistent with the Alfvén resonator, with the transmission efficiency through the ionosphere depending on frequency, and further being different for the two wave modes. Below this frequency (< 0.01 Hz) the mode structure is the same for both modes. However, the actual mode structure depends on the boundary conditions at the bottom of the surface-ionosphere waveguide, being different for open or perfectly reflecting boundary conditions. One feature missing for parallel propagation is the ``Hughes rotation,'' where the wave magnetic field below the ionosphere is rotated by 90 ° with respect to the wave magnetic field above the ionosphere. This appears to be a result of oblique propagation, with the fast mode being evanescent in the vertical direction when the mode is assumed to propagate across the ambient field. While some consideration must be given to the differences between parallel and oblique propagation, the results for the parallel case indicate that only low frequency waves would maintain consistent polarization through the ionosphere. The differences in attenuation and polarization as a function of frequency argue against the surface-ionosphere waveguide as being the path for transmitting signals such as changes in magnetospheric convection to lower latitudes.
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