Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985georl..12..749w&link_type=abstract
Geophysical Research Letters (ISSN 0094-8276), vol. 12, Nov. 1985, p. 749-752.
Astronomy and Astrophysics
Astronomy
13
Comet Tails, Cometary Atmospheres, Ion Motion, Solar Wind, Astronomical Models, Channel Flow, Comet Heads, Interplanetary Magnetic Fields, Ionospheres, Magnetic Effects, Rays, Comets, Magnetic Properties, Magnetic Effects, Models, Structure, Ions, Evolution, Ionosphere, Ionopause, Flux Ropes, Solar Wind, Interaction, Plasma, Collisions, Distance, Latitude, Gases, Production Rate
Scientific paper
The present model of the structure and evolution of cometary rays views this radiation as the channeled outflow of cometary ions from the ionosphere. While ions in the central tail ray flow down the channel formed by the tailward closing of the draped interplanetary field, ions in the side rays flow through magnetic flux ropes that become embedded in the cometary ionosphere through Kelvin-Helmholtz instability of the cometary ionopause. The flux ropes tunnel through the ionosphere, penetrate the ionopause at two points, and extend out into the solar wind on both sides of the comet. Differences in observed cometary ray structure are attributed to differences in the radial distance and ecliptic latitude of different comets at the time of observation.
Neugebauer Matthias
Sibeck David G.
Siscoe George L.
Wolff Richard S.
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