Magnetoseismology: Remote sensing of plasma density in the magnetosphere by ground magnetometer observations

Details Magnetoseismology: Remote sensing of plasma density in the magnetosphere by ground magnetometer observations Magnetoseismology: Remote sensing of plasma density in the magnetosphere by ground magnetometer observations

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsm42e..07c&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SM42E-07

Other

2752 Mhd Waves And Instabilities, 2768 Plasmasphere, 2794 Instruments And Techniques

Scientific paper

There has been significant progress in recent years in the methods estimating the density of magnetospheric plasma from the observations of ground magnetometer stations. These methods are the only known ways to remotely detect the mass density of magnetospheric plasma, and therefore they are complementary to other methods measuring the charge density. As in terrestrial seismology and helioseismology, there are two approaches to infer the density distribution in the magnetosphere. The first approach is the eigenmode method, which estimates the plasma density from the field line resonance frequencies observed by ground stations. In particular, the gradient technique that uses the data from two stations closely separated in the north-south direction has led to many successful results in observing field line resonances. This method has been used to demonstrate the depletion of the plasmasphere during strong magnetic storms. The second approach is the travel-time method that was conceived very recently. It is found that the preliminary impulse of sudden commencements propagates to low-latitude ground stations via MHD waves rather than the Earth-ionosphere waveguide. The travel time of preliminary impulses is well predicted by Tamao's MHD-wave model, and thus the arrival time of preliminary impulses can be used to infer the density distribution in the magnetosphere. We review the principles of both methods, the examples of how they help us understand the physics of the plasmasphere, and the possible future improvements in both techniques and observations.

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