Chorus Observations at Saturn

Details Chorus Observations at Saturn Chorus Observations at Saturn

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufm.p53d..02h&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #P53D-02

Physics

2756 Planetary Magnetospheres (5443, 5737, 6033), 2772 Plasma Waves And Instabilities (2471), 5719 Interactions With Particles And Fields, 5737 Magnetospheres (2756)

Scientific paper

Whistler mode chorus has been detected by the Radio and Plasma Wave Science (RPWS) Instrument during the majority of Cassini's first fifty orbits of Saturn. At Saturn, chorus is detected in two different regions. The most common observations are of chorus propagating away from Saturn's magnetic equator, suggesting a source near the magnetic equator. This chorus is usually detected for many hours, is only observed below half the electron cyclotron frequency, occurs primarily from L shells of about 5 to 8, and shows no obvious correlation with Saturn latitude or local time. Higher resolution measurements show that the fine structure of this chorus consists of larger time scales (tens of seconds to minutes) than detected at the Earth (< 1 second). The second region of chorus detected at Saturn is in association with local plasma injections. For many of the plasma injection events, intense chorus emissions are detected both above and below half the electron cyclotron frequency, with a gap in the emission at half the cyclotron frequency. This chorus also shows fine structure at a much smaller time scale (< 1 second), and overall, the structure of the chorus appears similar to chorus detected at the Earth. The properties and characteristics of the chorus detected during the first fifty orbits of Cassini will be discussed, and the similarities and differences of the two types of chorus detected at Saturn will be examined.

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