Magnetospheric interaction with Triton's ionosphere

Details Magnetospheric interaction with Triton's ionosphere Magnetospheric interaction with Triton's ionosphere

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990georl..17.1661s&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 17, Sept. 1990, p. 1661-1664.

Mathematics

Probability

16

Electron Emission, Magnetospheric Electron Density, Planetary Ionospheres, Satellite Atmospheres, Triton, Voyager Project, Elastic Scattering, Inelastic Scattering, Ionopause, Planetary Magnetic Fields, Plasma Interactions

Scientific paper

The large electron densities measured by the Voyager radio occultation experiment are attributed to the precipitation of magnetospheric electrons with energy above 10 keV. Because the ionospheric electric Pedersen conductivity of Triton is about 10,000-20,000 mho and the Alfven conductance is about 3.5 mho, direct convective flow of plasma into the essentially infinitely conducting ionosphere is negligible. Magnetospheric electrons are transported to Triton's ionopause by curvature drift as a result of weak magnetic field line draping in a sub-Alfvenic plasma interaction with Triton. At the ionopause energetic electrons have a high probability of elastic and inelastic scattering and precipitate into the upper atmosphere. The average power dissipation is estimated to be about (2 - 3) x 10 to the 8th W.

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