Comment on the observed plasma densities in Jupiter's distant magnetotail (wake) - A possible explanation

Details Comment on the observed plasma densities in Jupiter's distant magnetotail (wake) - A possible explanation Comment on the observed plasma densities in Jupiter's distant magnetotail (wake) - A possible explanation

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984jgr....89.2369g&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 89, April 1, 1984, p. 2369, 2370.

Mathematics

Logic

8

Jupiter Atmosphere, Planetary Magnetic Fields, Planetary Magnetospheres, Plasma Density, Space Plasmas, Solar Planetary Interactions, Solar Wind, Voyager 2 Spacecraft, Jupiter, Magnetotail, Observations, Plasma, Density, Models, Flow, Hypotheses, Magnetic Properties, Features, Calculations, Parameters

Scientific paper

It is shown that the average plasma density observed by Voyager 2 inside the distant Jovian magnetotail may be explained by assuming that the tail boundary is a rotational discontinuity. It is assumed that the average solar wind inflow into the tail is determined by the Alfven velocity corresponding to the azimuthal component of the interplanetary magnetic field multiplied by the solar wind density and by a phenomenological parameter describing the efficiency of reconnection. It is also assumed that the inflow of the solar wind plasma in the initially almost void tail lobes results in solar wind protons becoming the dominant species in the tail at a distance much less than the Jupiter-Saturn distance. An approximate analytic formula for the average tail plasma density at a given point is presented.

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