Charge exchange avalanche at the cometopause

Details Charge exchange avalanche at the cometopause Charge exchange avalanche at the cometopause

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987georl..14.1174g&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 14, Nov. 1987, p. 1174-1177.

Physics

25

Charge Exchange, Cometary Atmospheres, Plasma Dynamics, Solar Protons, Solar Wind, Heavy Ions, Two Fluid Models, Comets, Plasma, Ions, Distance, Comae, Size, Thickness, Boundaries, Spacecraft Observations, Models, Halley, Parameters, Calculations, Charged Particles, Flow, Protons, Solar Wind, Velocity, Distribution, Photoionization, Temperature

Scientific paper

A sharp transition from a solar wind proton dominated flow to a plasma population primarily consisting of relatively cold cometary heavy ions has been observed at a cometocentric distance of about 160,000 km by the VEGA and GIOTTO missions. This boundary (the cometopause) was thought to be related to charge transfer processes, but its location and thickness are inconsistent with conventionally estimated ion - neutral coupling boundaries. In this paper a two-fluid model is used to investigate the major physical processes at the cometopause. By adopting observed comet Halley parameters the model is able to reproduce the location and the thickness of this charge exchange boundary.

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