Other
Scientific paper
Jul 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jgr....9510711p&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 95, July 1, 1990, p. 10711-10716.
Other
1
Bow Waves, Comet Tails, Electron Density Profiles, Giacobini-Zinner Comet, Magnetic Flux, Plasma Dynamics, Cometary Atmospheres, Flow Geometry, Interplanetary Magnetic Fields, Solar Wind, Thermal Noise, Comets, Giacobini-Zinner, Comet Tails, Structure, Magnetic Properties, Flow, Geometry, Spacecraft Observations, Ice Mission, Flux, Pressure, Magnetic Field, Electrons, Density, Diagrams, Ions, Heat, Friction, Mass Loading, Solar Wind, Ionosphere, Plasma
Scientific paper
The structure of Comet Giacobini Zinner's magnetic tail is interpreted in terms of a flow geometry similar to that proposed for the Venus wake. It is suggested that the two-step shape of the magnetic field profile obtained from the ICE measurements across each lobe of the magnetic tail of that comet is due to the different entry of interplanetary magnetic fluxes into that region. The low (about 30 gamma) intensity outer wings of the magnetic field profile result from magnetic fluxes convected by the mass-loaded shocked solar wind that enters the tail from the polar boundary of the comet's magnetic cavity. The high (about 60 gamma) intensity inner parts of the lobes result, on the other hand, from the compression that this flow produces on interplanetary magnetic field lines that have slipped past the polar boundary of the cavity after draping around the comet. The latter magnetic fluxes are not convected by the local plasma, but forced to accumulate around the central plasma tail that extends behind the comet.
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