Mapping the Location and Structure of the Plasmapause Using Geomagnetic Field Line Resonances

Details Mapping the Location and Structure of the Plasmapause Using Geomagnetic Field Line Resonances Mapping the Location and Structure of the Plasmapause Using Geomagnetic Field Line Resonances

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm11a0781m&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SM11A-0781

Physics

2730 Magnetosphere: Inner, 2731 Magnetosphere: Outer, 2752 Mhd Waves And Instabilities, 6939 Magnetospheric Physics

Scientific paper

Ultra-low frequency (ULF) plasma waves distribute energy of solar wind origin throughout the Earth's magnetosphere and down to the ground, where they are recorded as pulsations of the geomagnetic field. The waves propagate in the fast magnetosonic mode within the magnetosphere and may couple to cavity or waveguide modes or shear transverse mode field line eigenoscillations. Ground magnetometer arrays can therefore be used to examine properties of the magnetospheric plasma, providing an important complement to VLF and spacecraft studies. We present examples illustrating mapping of the magnetospheric plasma mass density from L=2.6 through to L>10. This includes quiet days when no plasmapause was present, and storm cycles when we can monitor the evolution of the dayside plasmapause location and shape. We also examine the response to solar wind pressure changes that appear to cause plasmapause motions on a time scale of about an hour. Finally, we discuss opportunities for exploring the plasma mass loading and its temporal variation by comparing ULF and VLF measurements.

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