Comparison of low frequency equatorial waves at Earth and Saturn: Polar and Cassini observations

Details Comparison of low frequency equatorial waves at Earth and Saturn: Polar and Cassini observations Comparison of low frequency equatorial waves at Earth and Saturn: Polar and Cassini observations

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm43b..08h&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM43B-08

Physics

2772 Plasma Waves And Instabilities (2471), 2774 Radiation Belts, 5737 Magnetospheres (2756), 6984 Waves In Plasma (7867), 7867 Wave/Particle Interactions (2483, 6984)

Scientific paper

Low-frequency electromagnetic emissions are often detected near the Earth's geomagnetic equator. Recent studies show that these fast magnetosonic equatorial waves may accelerate electrons and can thus potentially play an important role in radiation belt dynamics. The Polar Plasma Wave Instrument (PWI) often detected these waves near the geomagnetic equator. These emissions were usually detected below a few hundred Hz and showed a wide range of frequency structure, from macroscopic (funnel-shaped spectrum) to finer (narrow frequency bands with a spacing of only a few Hertz). The Cassini spacecraft, just finishing its four year prime mission, often detects low frequency emissions (<100 Hz) near the Saturnian magnetic equator. Unlike the fast magnetosonic waves at Earth, equatorial waves at Saturn are primarily electrostatic and show little fine structure. These emissions are detected from about 6 to 10 Saturn radii and are often accompanied by enhanced electron cyclotron harmonic (ECH) emissions. A survey of properties of each of these emissions will be presented and the similarities and differences will be discussed.

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