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Energetic oxygen and sulfur ions in the Jovian magnetosphere

Thesis/Dissertation ·
OSTI ID:6213098
Observations of 1 to 20 MeV/nuc oxygen, sodium, and sulfur ions in the Jovian magnetosphere are reported. Measurements made by the Cosmic Ray Subsystem on Voyager 1 and 2 are used to calculate abundances and energy spectra in the region from 5 to 20 Jovian radii (R/sub J/). The phase space density of the oxygen ions calculated from the spectra has a positive radial gradient between 6 and 17 R/sub J/, indicating an inward diffusive flow. The diffusion coefficient upper limit at 9 R/sub J/ is approx. 10/sup -5/s/sup -1/. This limit, combined with the analysis of voyager plasma observations by Siscoe et al. (1981), implies an upper limit to the mass loading rate near lo of approx. 10/sup 28/ ions/s. The energetic oxygen lifetime is within an order of magnitude of the strong pitch-angle diffusion lifetime in this region, with the largest total numbers of particles lost between 7.5 and 12.5 R/sub J/. It is shown that the losses are not due to geometric absorption by lo, absorption by dust grains, or energy loss in the plasma of the inner magnetosphere, and it is therefore postulated that the primary loss mechanism is pitch-angle scattering into the loss cone. The power delivered to the Jovian atmosphere by oxygen and sulfur ions with magnetic moments greater than 70 MeV/nuc-G (E greater than or equal to 0.3 MeV/nuc at 10 R/sub j/), scattered into the loss cone between 6 and 17 R/sub j/, is approx. 5 x 10/sup 12/ W; a power comparable to the approx. 1.2 x 10/sup 13/W required to produce the auroral emission observed by the ultraviolet spectrometer on Voyager. The measured dependence of the input power on magnetic moment threshold indicates that additional power is contributed by oxygen and sulfur ions with magnetic moments less than 70 meV/nuc-G.
Research Organization:
California Inst. of Tech., Pasadena (USA)
OSTI ID:
6213098
Country of Publication:
United States
Language:
English