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A.L. Graps (MPI-K), E. Gr\"un (MPI-K), H. Svedhem (ESTEC), M. Horanyi (LASP), A. Heck (MPI-K), H. Kr\"uger (MPI-K)
The story of the Jovian dust streams began in 1992 with Ulysses' Dust Detector observations of high rate bursts of submicron sized particles travelling in the same direction from a source in the Jovian system (Grün, E. et al., 1993). Observations since 1995 (Grün, E. et al., 1996) from the Galileo Dust Detector instrument have revealed more dust streams. The origin of the dust streams has not been resolved, however. Throughout the last six years, investigators have proposed several dust sources (with models) for the streams: Jupiter's main ring/halo, Jupiter's gossamer ring, comet Shoemaker-Levy 9, and Io's volcanoes. Previous investigations have ruled out all of these but Jupiter's gossamer ring and Io's volcanoes, and for these latter two sources, the investigators have not been able to determine conclusively which of these two possibilities were the source of the particles. Now we show here, from time-frequency analysis methods, that the data is best matched by Io being the source of the Jovian dust streams.
\noindent Grün, E., et al., Discovery of Jovian dust streams and interstellar grains by the Ulysses spacecraft, {\it Nature}, {\it 362}, 428-430, 1993.
\noindent Grün, E., et. al., Constraints from Galileo observations on the origin of Jovian dust streams, {\it Nature}, {\it 381}, 395-398, 1996.
The author(s) of this abstract have provided an email address for comments about the abstract: Amara.Graps@mpi-hd.mpg.de