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A. L. Graps (IFSI, Rome, Italy), E. Grün, H. Krueger (MPI-K, Heidelberg, Germany), Galileo Dust Team
Of the several populations of dust in the Jovian environment, the most abundant by far is the Jovian dust streams. The Jovian dust streams are dominated by high-speed (greater then 200 km/sec) collimated streams of submicron-sized particles traveling from Jupiter's moon Io, in particular, from Io's volcanoes. From this source, the Jovian magnetosphere is mass-loaded at a rate approximately 6 g/sec to 6 kg/sec, of which some dust escapes into the interplanetary space and beyond. Upon applying criteria for ``dust-in-plasma" and ``dusty-plasma", using the dust grain size, Debye length, and dust intergrain distance for the Jovian dust stream particles, we find that, in the part of the Jovian magnetosphere starting from 10-15 Jovian radii, collective effects might be important. From roughly this distance, a dusty plasma, rather than a dust-in-plasma fits the Jupiter magnetospheric conditions. The specific Galileo orbits: E4, G7, G8, C21, highlight the time-variability of the process. Collective interactions occur when self-generated fields of the particles take over a correlative role, therefore the dust particles could behave differently from what would be expected from single particle physics. More complex frequencies and waves should be seen. In this presentation, I will show how to distinguish between dust-in-plasma and dusty plasma regimes and why current Galileo dust stream data hints at dusty plasma collective behavior.
The author(s) of this abstract have provided an email address for comments about the abstract: amara.graps@ifsi.rm.cnr.it
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Bulletin of the American Astronomical Society, 35 #4
© 2003. The American Astronomical Soceity.