DPS 2001 meeting, November 2001
Session 50. Solar System Dust
Oral, Chair: F. Spahn, Friday, November 30, 2001, 5:50-6:40pm, Regency GH

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[50.02] Io Revealed in the Jovian Dust Streams

A. L. Graps, E. Gruen, H. Krueger (MPI-K, Heidelberg, DE), M. Horanyi (LASP, Boulder, CO), H. Svedhem (ESTEC, Noordwijk, Netherlands), Galileo Dust Team, Cassini Dust Team

The Jovian dust streams are high-speed bursts of submicron-sized particles travelling in the same direction from a source in the Jovian system. Since their discovery in 1992, they have been observed by three spacecraft: Ulysses, Galileo and Cassini. The work presented here describes an emerging electrodynamical picture of the Jovian dust streams. The source of the Jovian dust streams is Jupiter's moon, Io, in particular, dust from Io's volcanoes. Charged Io dust, travelling on trajectories from Io's location, is shown to have some particular signatures in frequency space and in real space. The frequency-transformed Galileo dust stream measurements show different signatures, varying, orbit-to-orbit during Galileo's first 29 orbits around Jupiter. Time-frequency analysis demonstrates that Io is a localized source of charged dust particles. In real space, aspects of the particles' dynamics can be seen in the December 2000 joint Galileo-Cassini dust stream measurements. To match the travel times, the smallest dust particles could have the following range of parameters: radius: 6 nm, density: 1.35-1.75 g-cm-3, sulfur charging conditions, which produce dust stream speeds: 220/450 km-sec-1 (Galileo/Cassini) and charge potentials: 5.5/6.3 V (Galileo/Cassini).

Funding provided by the Deutsches Zentrum für Luft-und Raumfahrt E.V. (DLR), and the Deutsche Forschungsgemeinschaft (DFG).

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The author(s) of this abstract have provided an email address for comments about the abstract: Amara.Graps@mpi-hd.mpg.de

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