Narrowband Electromagnetic Emissions at Saturn Revisited: Cassini Observations

Details Narrowband Electromagnetic Emissions at Saturn Revisited: Cassini Observations Narrowband Electromagnetic Emissions at Saturn Revisited: Cassini Observations

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsm12a..05k&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SM12A-05

Astronomy and Astrophysics

Astronomy

2756 Planetary Magnetospheres (5443, 5737, 6030), 2772 Plasma Waves And Instabilities, 5737 Magnetospheres (2756), 6954 Radio Astronomy, 7534 Radio Emissions

Scientific paper

Voyager observations revealed the existence of a complex set of narrowband electromagnetic emissions at Saturn in the frequency range of 3 to 30 kHz. These were found to be generated by mode conversion from electrostatic upper hybrid waves into ordinary mode electromagnetic waves which could freely propagate from the source. The frequency spacings of the narrowband emissions near the electron cyclotron frequency at Tethys, Dione, and Rhea suggested that these bands may be produced near these moons as part of their interaction with Saturn's magnetosphere. Cassini has now been in orbit at Saturn for seven months and has had an opportunity to further explore the low-frequency narrowband emissions. Similar emissions found over the ring system have been shown to be propagating in the Z-mode [Farrell et al., submitted, J. Geophys. Res., 2005], hence, would not propagate far from Saturn. However, other narrowband emissions observed by Cassini appear to be similar to those discovered with Voyager. Most of these, however, are found in the solar wind upstream of Saturn's bow shock. These emissions typically consist of a single band in the frequency range of ~6 to 8 kHz but sometimes are seen outside this range. More complex sets of bands are also seen, although not as often. In this paper we examine the new observations in an attempt to further understand the source of these emissions.

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