Hostname: page-component-848d4c4894-8bljj Total loading time: 0 Render date: 2024-07-06T17:48:16.167Z Has data issue: false hasContentIssue false

Objective Prism Spectroscopy of the Tail of Comet Austin 1982 G

Published online by Cambridge University Press:  12 April 2016

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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
Copyright
Copyright © Reidel 1984

References

Arpigny, C: 1965, Mem. Acad. R. Belgique, Coll. 8 35, Fasc. 5.Google Scholar
Huebner, W.F., and Giguere, P.T.: 1980, Astrophys. J. 238, 753.Google Scholar
Jockers, K.: 1982, ESO Workshop on Comet Halley (ed. Veron, P., Festou, M., Kjär, K.), p. 149.Google Scholar
Lamy, Ph.L., and Koutchmy, S.: 1982, ESO Workshop on Comet Halley (ed. Veron, P., Festou, M., Kjär, K.), p. 242.Google Scholar
Swings, P., and Page, Th,: 1950, Astrophys. J. 111, 530.Google Scholar
Wyckhoff, S., and Wehinger, P.A.: 1976a, Astrophys. J. 204, 604.Google Scholar
Wyckhoff, S., and Wehinger, P.A.: 1976b, Astrophys. J. 204, 616.Google Scholar