Comet ion formation and dynamics

Details Comet ion formation and dynamics Comet ion formation and dynamics

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ncgb.conf..171w&link_type=abstract

IN: Workshop on the Need for Coordinated Ground-Based Observations of Halley's Comet, Paris, France, April 29, 30, 1982, Proceed

Astronomy and Astrophysics

Astronomy

1

Atmospheric Ionization, Cometary Atmospheres, Plasma Dynamics, Solar Activity Effects, Astronomical Models, Cometary Magnetospheres, Halley'S Comet, Magnetic Fields, Magnetohydrodynamic Waves, Magnetosheath, Solar Wind

Scientific paper

Solar photon and proton ionization may well supply average ion fluxes, but closer observation correlated with solar-wind conditions is needed to distinguish intrinsic mechanisms such as auroral discharges or ionizing flow instability from the variable solar-wind 'snow-plough'. Under steady conditions, the expected plasma flow is relatively smooth, varying over scales much larger than ion gyro-radii (the effective m.f.p.), and even the plasma bow shock would have limited physical significance. The interplanetary field may be pictured as draping around the comet head, but Alfven's (1957, 1981) picture needs modifying to include slipping over into the tail. The concept of one-fluid plasma picking up fresh cometary ions is challenged, because relative drifts in the draped fields are inevitably major. Structures and tail rays, as enhancements of density, drift towards the tail axis across the draped field. Magnetic forces become appreciable at order ten times the ionosphere radius, so the transition region of induced currents and fields should be very broad, unlike the Venus magnetosheath. Time-sequenced observations at around 10-minute intervals are needed for tracing the evolution of ion structures in a Halley-sized comet.

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