Cassini Observations of Jovian Anomalous Continuum

Details Cassini Observations of Jovian Anomalous Continuum Cassini Observations of Jovian Anomalous Continuum

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsm41a..08h&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SM41A-08

Physics

2708 Current Systems (2409), 2784 Solar Wind/Magnetosphere Interactions, 5737 Magnetospheres (2756), 2431 Ionosphere/, Agnetosphere Interactions (2736) : : : : : : : : : : : : : : :, 6939 Magnetospheric Physics, 6984 Waves In Plasma

Scientific paper

Jupiter produces a wide range of radio emissions, including low-frequency emissions in the 100-Hz to 30-kHz range. These low-frequency emissions have a variety of characteristics, and include narrowband tones, quasi-periodic bursts, and three types of continuum like emissions (escaping, trapped, and anomalous continuum). Jovian anomalous continuum emission is usually observed below 20 kHz, has a negative frequency drift with a long duration (many hours), and a clock-like behavior (typically ten hours). Previous studies with the Ulysses spacecraft have suggested that anomalous continuum emission is related to the quasi-periodic radio bursts, solar wind pressure, and that it is not the same emission as Jovian escaping continuum. The Cassini flyby of Jupiter in December 2000 provided a new opportunity to observe this low-frequency radiation. Nearly continuous data has been obtained by the Radio and Plasma Wave System (RPWS) from early 2000 to the present, and many examples of these low-frequency emissions have been detected. The distance between Cassini and Jupiter has ranged from about 137 to over 5000 Jovian radii. We will examine the Cassini observations of these emissions, compare them to the earlier results from Voyager and Ulysses, and discuss the generation mechanisms that have been proposed for these emissions.

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