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Energetic-ion acceleration and transport in the upstream region of Jupiter : Voyager 1 and 2.

Author
Zwickl, R. D.
Published
JAN 1, 1982.
Physical Description
1 electronic document
Additional Creators
Lepping, R. P., Krimigis, S. M., Baker, D. N., and Carbary, J. F.
Online Version

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Summary
Long-lived upstream energetic ion events at Jupiter appear to be very similar in nearly all respects to upstream ion events at Earth. A notable difference between the two planetary systems is the enhanced heavy ion compositional signature reported for the Jovian events. This compositional feature has suggested that ions escaping from the Jovian magnetosphere play an important role in forming upstream ion populations at Jupiter. In contrast, models of energetic upstream ions at Earth emphasize in situ acceleration of reflected solar wind ions within the upstream region itself. Using Voyager 1 and 2 energetic ( approximately 30 keV) ion measurements near the magnetopause, in the magnetosheath, and immediately upstream of the bow shock, the compositional patterns are examined together with typical energy spectra in each of these regions. A model involving upstream Fermi acceleration early in events and emphasizing energetic particle escape in the prenoon part of the Jovian magnetosphere late in events is presented to explain many of the features in the upstream region of Jupiter.
Other Subject(s)
Collection
NASA Technical Reports Server (NTRS) Collection.
Note
Document ID: 19830019675.
Accession ID: 83N27946.
DE82-019574.
NASA-TM-85179.
CONF-82058-3.
LA-UR-82-1914.
NAS 1.15:85179.
Symp. on Giant Planets and Their Satellites; 17-27 May 1982; Ottawa.
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