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Objective Prism Spectroscopy of the Tail of Comet Austin 1982 G

Published online by Cambridge University Press:  12 April 2016

K. Jockers  and
L.G. Balázs
K. Jockers
Affiliation:
Max-Planck-Institut für Aeronomie, D-3411 Katlenburg-Lindau, FRG, Visiting Astronomer at Observatorium Hoher List, Daun, FRG
L.G. Balázs
Affiliation:
Konkoly Observatorium, Budapest, Hungary

Abstract

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The main emissions of the cometary plasma tail are due to CO+ (400/402 and 425/427 nm) and H2O+ (aroud 650 nm). Emissions of CO2+ at 367 nm have also been observed (Swings and Page 1950). These ions relate much more directly to the presumed mother molecules of the cometary nucleus (like H2O, CO2, CO) than most strong emissions of the neutral cometary coma (Ruebner and Giguere, 1980, see also Jockers, 1982). Therefore it is important to determine column densities of cometary ions. So far only very few measurements of ion column densities are available (Wyckhoff and Wehinger, 1976a, b; Arpigny, 1965).

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 78: Astronomy with Schmidt-type telescopes , 1984 , pp. 237 - 239
Copyright
Copyright © Reidel 1984

References

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